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Published for SISSA by Springer Received: April 15, 2013

Revised: June 3, 2013 Accepted: June 5, 2013 Published: June 28, 2013

Cline Bhm,a,b P.S. Bhupal Dev,c Anupam Mazumdard,e and Ernestas Pukartasd

aInstitute for Particle Physics Phenomenology, University of Durham, Durham DH1 3LE, U.K.

bLAPTh, U. de Savoie, CNRS, BP 110, 74941 Annecy-Le-Vieux, France

cConsortium for Fundamental Physics, School of Physics and Astronomy, University of Manchester, Manchester M13 9PL, U.K.

dConsortium for Fundamental Physics, Lancaster University, Lancaster LA1 4YB, U.K.

eNiels Bohr Institute, Copenhagen University, Blegdamsvej-17, Copenhagen, Denmark

E-mail: mailto:[email protected]

Web End [email protected] , mailto:[email protected]

Web End [email protected] ,mailto:[email protected]

Web End [email protected] , mailto:[email protected]

Web End [email protected]

Abstract: We examine the possibility of a light (below 46 GeV) neutralino dark matter (DM) candidate within the 19-parameter phenomenological Minimal Supersymmetric Standard Model (pMSSM) in the light of various recent experimental results, especially from the LHC, XENON100, and Planck. We also study the extent of electroweak ne-tuning for such a light neutralino scenario in view of the null results from the searches for supersymmetry so far. Using a Markov Chain Monte Carlo likelihood analysis of the full pMSSM parameter space, we nd that a neutralino DM with mass [greaterorsimilar] 10 GeV can in principle still satisfy all the existing constraints. Our light neutralino solutions can be broadly divided into two regions: (i) The solutions in the 1030 GeV neutralino mass range are highly ne-tuned and require the existence of light selectrons (below 100 GeV) in order to satisfy the observed DM relic density. We note that these are not yet conclusively ruled out by the existing LEP/LHC results, and a dedicated analysis valid for a non-unied gaugino mass spectrum is required to exclude this possibility. (ii) The solutions with low ne-tuning are mainly in the 3046 GeV neutralino mass range. However, a major portion of it is already ruled out by the latest XENON100 upper limits on its spin-independent direct detection cross section, and the rest of the allowed points are within the XENON1T projected limit. Thus, we show that the allowed MSSM parameter space for a light neutralino DM below the LEP limit of 46 GeV, possible in supersymmetric models without gaugino mass unication, could be completely accessible in near future. This might be useful in view of the recent claims for positive hints of a DM signal in some direct detection experiments.

Keywords: Supersymmetry Phenomenology

ArXiv ePrint: 1303.5386

Open Access doi:http://dx.doi.org/10.1007/JHEP06(2013)113

Web End =10.1007/JHEP06(2013)113

Naturalness of light neutralino dark matter in pMSSM after LHC, XENON100 and Planck data

JHEP06(2013)113

Contents

1 Introduction 1

2 Electroweak ne-tuning 4

3 Parameters and constraints 6

4 Results 12

5 Conclusion 18

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1 Introduction

Low-scale Supersymmetry (SUSY) (see e.g., [1, 2]) is one of the most attractive candidates for New Physics beyond the Standard Model (SM). Apart from providing successful gauge coupling unication and a solution to the gauge hierarchy problem, it o ers a natural candidate for Dark Matter (DM) in our Universe in the form of the lightest supersymmetric particle (LSP). In the R-parity conserving Minimal Supersymmetric Standard Model (MSSM), the lightest neutralino (

e[notdef]01) is one of the most viable Weakly Interacting Massive Particle (WIMP) DM candidates (for a review, see e.g., [3, 4]). It can explain the observed

DM relic density, while predicting experimentally accessible direct and indirect detection rates, over a wide range of supersymmetric model parameters, some of which are already getting constrained from the ongoing direct searches for the supersymmetric particles at the Large Hadron Collider (LHC), in combination with other low-energy data (for a review, see e.g., [5]).

The recent hints of positive signals in three DM direct detection experiments, namely, DAMA [6, 7], CoGeNT [8] and CRESST-II [9], have generated a lot of interest in light WIMP candidates in the 550 GeV mass range. This interpretation is however challenged by the null results from various other direct detection experiments, most notably the latest XENON100 results [10], which provide the most stringent upper limits on the spin-independent WIMP-nucleon scattering cross section for m[notdef] > 7 GeV.1 Nonetheless, due to the relatively poor sensitivity of the XENON100 experiment in the very low WIMP mass regime, it is believed that an agreement between the positive and null sets of experimental results could be possible, if at all, only in this low mass region. Hence, it might be worthwhile examining the allowed MSSM parameter space to see if there exists a lower bound on the lightest neutralino mass irrespective of the direct detection results.

1More recently, the TEXONO experiment [11] has achieved slightly better sensitivity than XENON100 for m~ < 7 GeV.

The neutralino mass eigenstates in the MSSM result from mixing of the neutral bino (

eB), wino ( fW 0) and higgsinos ( eH0d,

eH0u). This mixing is determined by the MSSM tan parameter and the bino, wino and higgsino mass parameters M1, M2 and [notdef], respectively. In the SUSY models with gaugino mass unication at the Grand Unied Theory (GUT) scale, a relation between the bino and wino mass follows at the electroweak scale: M1 = 53 tan2 W M2 0.5M2 (see e.g., [12]) which, after mixing, translates into a chargino

neutralino mass relation. Therefore, a lower limit on the lightest neutralino (

e[notdef]01) mass of about 46 GeV can be derived for these models from the Large Electron Positron (LEP)

chargino mass limit [13, 14], whereas in the constrained MSSM (cMSSM) [15] with both gaugino and sfermion mass unication, this limit increases to well above 100 GeV from the strong constraints set by the recent LHC data [5].

On the other hand, in a generic MSSM scenario without the assumption of gaugino mass unication, there is no general lower limit on the lightest neutralino mass [16]. The LEP limit on the invisible decay width of the SM Z boson applies to light neutralinos with a mass below mZ/2 = 45.6 GeV, but it depends on the Z

e[notdef]01

e[notdef]01 coupling which could be small or even zero, depending on the higgsino component of the neutralino. In such a case, light neutralinos are mainly constrained by the DM relic density measurement as well as by the collider and avor constraints on the SUSY parameter space. Assuming that the lightest neutralino is non-relativistic and provides the entire cold DM content of the Universe, while satisfying the LEP bounds on chargino and stau masses, ref. [17] obtained a lower bound of m[tildewide][notdef]

01 [greaterorsimilar] 18 GeV. This was relaxed to about 6 GeV without violating the LEP bounds and avor sector constraints in SUSY models with a pseudo-scalar Higgs boson (A)

mass mA < 200 GeV and a large tan [18, 19]. This was even further lowered to about3 GeV by allowing explicit CP violation in the MSSM Higgs sector [20].

Meanwhile, several new experimental results have been obtained at the LHC: (i) A new Higgs-like neutral scalar particle has been discovered [21, 22] with mass around 125 GeV which falls squarely within the MSSM-predicted range for the lightest CP -even neutral Higgs mass: mh 2 [115, 135] GeV (see e.g., [23]); (ii) The rare decay B0s ! [notdef]+[notdef] was

observed with a branching fraction of B(B0s ! [notdef]+[notdef]) = 3.2+1.51.2

[parenrightbig]

[notdef] 109 [24] which is

in agreement with the SM expectation, B(B0s ! [notdef]+[notdef])SM = (3.23 [notdef] 0.27) [notdef] 109 [25];

(iii) The lack of a SUSY signal at the ps = 7 and 8 TeV LHC has pushed the lower limits on the squark and gluino masses to about 1 TeV and beyond [26, 27]; (iv) Updated bounds have been obtained for the MSSM Higgs sector [2830]. All these new results have profound implications for a light neutralino scenario within the MSSM, and some of these aspects have already been investigated in a number of recent studies [3145]. The general conclusion is that light neutralino DM candidates with mass below about 15 GeV are severely constrained in generic MSSM scenarios (without gaugino mass unication).

Another important issue to be addressed in the light of the recent LHC results is the apparent little hierarchy problem, i.e., how does a multi-TeV SUSY particle spectrum conspire to give a weak-scale Z-boson mass and also a Higgs boson mass of 125 GeV? One way of analyzing this issue quantitatively is to evaluate the measure of electroweak ne-tuning (EWFT) by examining the minimization condition in the MSSM Higgs potential which determines the Z-boson mass [46, 47]. It is well-known that radiative corrections

JHEP06(2013)113

must play a crucial role in determining the allowed SUSY parameter space necessary to generate a 125 GeV Higgs boson mass, much larger than its tree-level prediction of mh mZ.

This in general can lead to a large ne-tuning. In addition to this, the requirement of a light neutralino DM will pose a challenge for any MSSM scenario, the severity of which is however strongly model-dependent. The naturalness of various SUSY models with a neutralino LSP has been analyzed in the literature (for an incomplete list, see [42, 4861], and references therein).

In this paper, we perform a dedicated study focusing on the naturalness of a light neutralino, and also examining how light the neutralino could be, after taking into account all the existing theoretical and experimental constraints. To perform such an analysis in the full 124-parameter MSSM is quite unrealistic, and hence, we need to make some well-motivated assumptions in order to reduce the number of parameters to a manageable level. Most of the earlier studies on SUSY focused on the cMSSM having only 5 parameters, assuming certain boundary conditions at the GUT-scale. However, in view of the latest null results from SUSY searches at the ps = 8 TeV LHC, the cMSSM seems too restrictive for low-scale SUSY phenomenology as the allowed cMSSM parameter space accessible to the ps = 14 TeV LHC is rapidly shrinking (for the latest global status, see e.g., ref. [62 64]). Therefore, in this paper we choose not to make any assumptions at the high scale, and focus only on the low-scale MSSM parameter space from a phenomenological point of view. More precisely, we consider a CP -conserving MSSM (i.e., with no new CP phases) with Minimal Flavor Violation [65] and with rst two generations of sfermions degenerate. This is widely known as the phenomenological MSSM (pMSSM) [66] (also known as SUSY without prejudice [67]) with 19 free parameters at the electroweak scale. We also study the level of ne-tuning for the light neutralino scenario in this context.

In order to e ciently explore the 19-dimensional pMSSM parameter space, we perform a Markov Chain Monte Carlo (MCMC) likelihood analysis (for a review, see e.g., [68]), with the priors chosen to focus on a light neutralino scenario with mass below the conservative LEP lower limit of 46 GeV. We include in our analysis the latest experimental results for SUSY searches from the LHC [26, 27] which now supersede the Tevatron results [69, 70], in addition to the existing LEP limits [13, 14], wherever applicable. We also include the latest astrophysical/cosmological constraints for a WIMP DM from the 9-year WMAP data [71] as well as the very recently released Planck data [72]. We further examine the allowed parameter space in the light of various recent results for DM direct detection, most notably the XENON100 limits [10], as well as the indirect detection results from Fermi-LAT data [73].

We nd that a light neutralino DM with mass as low as 10 GeV is still allowed in the pMSSM, while satisfying all the existing experimental constraints provided we only take the model-independent analysis results from LEP. (Including the LEP limits strictly applicable to gaugino-mass unication models allows only the solutions with m[tildewide][notdef]

01 > 30 GeV,

in agreement with previous results [33, 34].) However, such neutralinos which are required to be mostly bino-like are severely ne-tuned and require the existence of light sleptons below 100 GeV in order to provide an e cient annihilation channel to reduce the bino relic density to be consistent with the observed limit. A dedicated analysis of the LEP data in the context of a pMSSM scenario could eliminate this region completely. On the other hand, low

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01 = 45 GeV where the resonant annihilation via the s-channel Z-exchange is possible for the neutralino with a non-negligible higgsino component. However, such regions are mostly excluded by the recent XENON100 limits on the spin-independent DM-nucleon scattering cross section, and the remaining such points are well within the reach of the XENON1T [74] and LUX [75] projected limits.

Our paper is organized as follows: in section 2, we briey discuss the electroweak ne-tuning measure. In section 3, we list all the pMSSM parameters and their scan ranges, and also summarize all the relevant experimental constraints used in our numerical analysis. In section 4, we present our scan results and discuss their implications for a light neutralino DM. Finally, our conclusions are given in section 5.

2 Electroweak ne-tuning

To quantify the amount of ne-tuning in the electroweak symmetry breaking (EWSB) sector of the MSSM, it is su cient for us to analyze the tree-level MSSM scalar potential. Since it allows only charge-conserving vacua, we only have to minimize the scalar potential for the neutral scalar elds [1]:

V = (m2Hu + [notdef]2)[notdef]H0u[notdef]2 + (m2Hd + [notdef]2)[notdef]H0d[notdef]2

B[notdef](H0uH0d + H.c.) + 18(g2 + g[prime]2)([notdef]H0u[notdef]2 [notdef]H0d[notdef]2)2 , (2.1)

where [notdef] is the SUSY-preserving bilinear Higgs superpotential parameter, mHu,d and B are

the soft scalar masses and the bilinear coupling in the SUSY-breaking sector respectively, and g, g[prime] the SU(2)L and U(1)Y gauge couplings, respectively. After minimization, we obtain the well-known relation for the Z-boson mass:

m2Z2 =

ne-tuning regions can be obtained around m[tildewide][notdef]

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m2Hd m2Hu tan2 tan2 1

[notdef]2, (2.2)

where tan = vu/vd is the ratio of the vacuum expectation values (vevs) of the two Higgs doublet elds Hu and Hd respectively, It is clear from eq. (2.2) that a cancellation of the terms on the right hand side (RHS) is required in order to obtain the measured value of mZ = 91.2 GeV [5] especially if the mass parameters on the RHS are orders of magnitude larger than the weak scale which indeed seems to be the case, given the current experimental status of the direct SUSY searches [26, 27]. Thus naively speaking, the weak scale value of [notdef][notdef][notdef] can be used as a measure of ne-tuning in the MSSM.

A more sophisticated way to quantify the degree of EWFT is by using log-derivatives [47]:

pi = [vextendsingle][vextendsingle][vextendsingle][vextendsingle]

, (2.3)

where pis are the parameters that determine the observable Z-mass at tree-level. From eq. (2.2), we have pi = [notdef][notdef]2, b, mHu, mHd[notdef] (with b B[notdef]), and the total measure of the

EWFT is dened as

tot =

q( [notdef]2)2 + ( b)2 + ( m2Hu)2 + ( m2Hd)2, (2.4)

@ ln m2Z(pi) @ ln pi

[vextendsingle][vextendsingle][vextendsingle][vextendsingle]

pi m2Z

@m2Z @pi

with the individual pis given by [76]

[notdef]2 = 4[notdef]2 m2Z

1 + m2A + m2Z

m2Atan2 2

b =

1 + m2A m2Z

tan2 2 ,

m2Hu =

[vextendsingle][vextendsingle][vextendsingle][vextendsingle]

2 cos 2 +

m2A m2Z

cos2

[notdef]2 m2Z

[vextendsingle][vextendsingle][vextendsingle][vextendsingle]

1 1cos 2 +m2A + m2Z

m2Atan2 2

m2Hd =

[vextendsingle][vextendsingle][vextendsingle][vextendsingle]

2 cos 2 +

m2A m2Z

sin2

[notdef]2 m2Z

[vextendsingle][vextendsingle][vextendsingle][vextendsingle]

1 + 1cos 2 +m2A + m2Z

m2Atan2 2

. (2.5)

Here m2A = B[notdef](tan + cot ) is the MSSM pseudo-scalar Higgs mass, and we have assumed tan > 0. Values of tot 1 indicate signicant ne-tuning. Note that in the

decoupling limit with mA mZ and with large tan , the quantities m2Hu and m2Hd in

eq. (2.5) are small, and

[notdef]2 [similarequal]

4[notdef]2 m2Z

. (2.6)

Thus in the limit of large tan , we recover the naive result that ne-tuning increases with increasing [notdef][notdef][notdef].

We should note here that including loop corrections to eq. (2.2), one nds the largest contribution to be coming from the (s)top loop which feeds into the soft mass of the Higgs [12]:

m2Hu =

3y2t82 (m2[tildewide]tL

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, b [similarequal]

4m2A m2Z tan2

+ m2[tildewide]tR

+ [notdef]At[notdef]2) log [parenleftbigg]

, (2.7)

where yt is the top-quark Yukawa coupling, At is the third-generation A-term in the SUSY-breaking sector, and is some high scale where the stop masses m[tildewide]tL,R

m[tildewide]t

are generated from the SUSY-breaking mechanism. Even for a low-scale SUSY-breaking scenario (such as gauge mediation), this requires a ne-tuning of at least a few percent in order to get the ob-served Z-mass and it becomes worse for heavy stop masses [77]. A heavy physical stop mass m[tildewide]t

[greaterorsimilar] 500 GeV is anyway required to provide large enough radiative corrections to the light CP -even Higgs mass to raise it to the vicinity of 125 GeV from its tree-level value mZ [12]:

m2h0 =

3m4t 162v2

X2t12m[tildewide]tLm[tildewide]tR[parenrightBigg][bracketrightBigg]

, (2.8)

where Xt = At [notdef] cot is the stop mixing parameter. A ne-tuning measure mh for the

Higgs mass can be dened analogous to eq. (2.3), and for a particular choice of some of the SUSY parameters, it was found that mh > 75 (100) in order to achieve a Higgs mass of 124 (126) GeV and the corresponding stop mass is always heavier than 300 (500) GeV [78].

The ne-tuning due to eqs. (2.7) and (2.8) could in principle be added in quadratures to our total ne-tuning parameter dened by eq. (2.4), but since their specic values are scale-dependent2 and adds to some arbitrariness in its denition, we do not include them in our analysis.

2The SUSY-scale by convention is usually taken to be the geometric mean of the two stop masses.

"log

m2[tildewide]t

L m2[tildewide]t

Rm4t

[parenrightBigg]+ X2t m[tildewide]tL m[tildewide]tR

Parameter Description Prior Range tan Ratio of the scalar doublet vevs [1, 60]

[notdef] Higgs-Higgsino mass parameter [3, 3] TeV

MA Pseudo-scalar Higgs mass [0.3, 3] TeV M1 Bino mass [0.5, 0.5] TeV

M2 Wino mass [1, 1] TeV

M3 Gluino mass [0.8, 3] TeV m[tildewide]qL

First/second generation QL squark [0, 3] TeV m[tildewide]uR

First/second generation UR squark [0, 3] TeV m

edR First/second generation DR squark [0, 3] TeV m[tildewide][lscript]LFirst/second generation LL slepton [0, 3] TeV m[tildewide]eR

First/second generation ER slepton [0, 3] TeV m

eQ3L Third generation QL squark [0, 3] TeV m[tildewide]tR

Third generation DR squark [0, 3] TeV m[tildewide]L3L

m[tildewide]bR

m[tildewide]R

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Third generation UR squark [0, 3] TeV

Third generation LL slepton [0, 3] TeV

Third generation ER slepton [0, 3] TeV At Trilinear coupling for top quark [10, 10] TeV

Ab Trilinear coupling for bottom quark [10, 10] TeV

A Trilinear coupling for -lepton [10, 10] TeV

Table 1. The pMSSM parameters and their range of values used in our numerical analysis.

3 Parameters and constraints

We consider the pMSSM with 19 free parameters at the SUSY scale, as shown in table 1. We further assume that the lightest neutralino is the LSP, and our goal is to examine how light and natural the neutralino could be while satisfying all the existing theoretical and experimental constraints on the MSSM parameter space. In particular, we focus on the lightest neutralino masses below the LEP limit of 46 GeV [13, 14] which is strictly valid assuming gaugino mass unication at the GUT-scale. We perform a numerical scan over the 19-dimensional pMSSM parameter space using a MCMC-based likelihood analysis for a light neutralino with the prior ranges given in table 1. These particular ranges are chosen in order to economize the scan time and to focus only on the SUSY parameter space not yet disfavored by the combined direct search results from the LEP [13, 14], Tevatron [69, 70] and LHC [26, 27], as discussed later in this section. For the SM parameters s(mZ), em(mZ), mW , mt and mb, we use the standard values as given in ref. [5].

Apart from the direct collider constraints on the sparticle masses, there exist various theoretical and experimental constraints which must be imposed on the pMSSM parameter

space in our analysis. As a standard theoretical requirement, our sparticle spectrum for each allowed point in the parameter space must be tachyon-free and should not lead to color- and charge-breaking minima in the scalar potential [79]. We also require that the scalar potential is bounded from below and is consistent with electroweak symmetry breaking. From the radiative electroweak symmetry breaking arguments, we can restrict the tan parameter to be roughly between 160, as given in table 1.

The various experimental constraints from direct collider searches, Higgs and avor sectors, and astrophysical/cosmological data used in our analysis are summarized below.

Invisible Z-decay width

The precise measurement of the Z-boson decay width at LEP: totZ = 2495.2[notdef]2.3 MeV [80]

puts severe constraints on light neutralinos and charginos with mass < mZ/2. From

the LEP measurements of the invisible decay width of the Z-boson: invZ = (499.0 [notdef] 1.5) MeV [80], the parameter space for the lightest neutralino in our case is restricted to mostly gaugino-like scenarios ([notdef][notdef][notdef] M1,2) since the neutralino coupling to Z is only via its

higgsino component. The allowed fraction of the higgsino component for a given neutralino mass can be calculated using the following expression for the partial decay width of the Z-boson to neutralinos [81]:

(Z !

e[notdef]01

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e[notdef]01) (Z !

) =2 1

4m2[tildewide][notdef]0

(OL11)2+(OR11)2

6m2[tildewide][notdef]0

[bracketrightBigg]

(3.1)

m2Z

!1/2[bracketleftBigg]1

m2[tildewide][notdef]01 m2Z

[parenrightBigg]

m2Z

1 OL11OR11

where (Z !

) = (501.62[notdef]0.10) MeV is the SM contribution to its invisible decay width

(for 3 neutrino species). The components OL,Rij are dened as

OLij =

2Ni3N j3 +

2Ni4N j4 , ORij = OLij

(3.2)

with Nij measuring the gaugino-Higgsino mixing:

e[notdef]0i =

Xk=1 Nik

eH0d). (3.3)

Using the LEP measurement of the invisible Z-decay width, the following constraint can be derived:

(Z !

e[notdef]0i

e 0k, where

e 0 = (

eB,

fW 0,

eH0u,

e[notdef]0j) < 3 MeV if (m[notdef]i + m[notdef]j) < mZ (3.4)

Note that this constraint should apply to all light neutralinos satisfying this condition, not just the LSP (i = j = 1 in eq. (3.4)). However, it is unlikely that decays such as Z !

e[notdef]02

e[notdef]01

will be kinematically allowed, and in such cases,

e[notdef]02 will mostly decay to visible nal states.

e j are not kinematically allowed for the parameter space examined here, and hence, they do not contribute to the purely invisible width of the Z-boson.

Similarly, the decays Z !

e i

Exclusion limits from collider searches

The experimental lower limits on the sparticle masses are usually quoted assuming gaugino and/or sfermion mass universality at the GUT scale. In a generic MSSM setup, most of these constraints can be relaxed, or even circumvented, for example in case of small mass splitting with the LSP or in case of small couplings to the SM vector bosons. Since we are interested in light neutralino LSPs here, we must carefully interpret the direct search limits in order to be able to include all the allowed pMSSM parameter space.

Neutralino. As already mentioned in section 1, there are no rigorous lower limits on the neutralino masses in the MSSM from direct collider searches. The LEP limits [13, 14, 82]

m[tildewide][notdef]

01 > 46 GeV, m[tildewide][notdef]

02 > 62.4 GeV, m[tildewide][notdef]

03 > 99.9 GeV, m[tildewide][notdef]

04 > 116.0 GeV (3.5)

were derived assuming gaugino mass unication at the GUT scale, and hence, relating the neutralino mass to the chargino mass. Moreover, for a (mostly) bino-like neutralino, which is required to be the case for m[tildewide][notdef]

01 < mZ/2 in order to avoid the Z-width constraint, its production via s-channel exchange of Z/ is (negligible) absent. The t-channel production cross-section via selectron exchange is also expected to be small for selectron masses above the LEP limit (see below). Thus, we can easily satisfy the LEP upper limits on the neutralino pair-production cross sections (e+e !

e[notdef]0j) [82, 83] for a mostly bino-like neutralino LSP. Similarly, the Tevatron [84] and LHC [85] SUSY searches for nal states involving Z-bosons cannot constrain a bino-like neutralino.

Chargino. Charginos can be pair-produced at LEP via s-channel exchange of Z/ or t-channel exchange of electron-sneutrino, with destructive interference. It dominantly decays to [lscript]

e , if kinematically allowed. If not, the three-body decay to f f[prime] e[notdef]0i via virtual W -boson or sfermions becomes important in which case, the nal state fermions (f, f[prime]) are dominantly leptonic (hadronic) if the sleptons are light (heavy). From the combined searches in fully-hadronic, semi-leptonic and fully-leptonic decay modes, LEP has derived a general lower limit of 103.5 GeV [13, 14] which is valid for pMSSM as well, except in corners of phase space where (i) the detection e ciencies are reduced, e.g., when the mass di erences m+ =

m[tildewide][notdef]

are very small (below a few GeV); or (ii) the chargino production cross section is suppressed, e.g., when the electron sneutrino mass is small, thus leading to a destructive interference between s- and t-channel Feynman diagrams. Dedicated searches for such scenarios have also been performed. For instance, for small m+ < 3 GeV but with large sneutrino mass, the limit becomes m[tildewide][notdef]

1 > 91.9 GeV for degeneracy in the gaugino region ([notdef]M1[notdef] [notdef]M2[notdef] [notdef][notdef][notdef]) while m[tildewide][notdef]

> 300 GeV. For smaller sneutrino masses, the sensitivity decreases due to the reduced pair production cross section and also due to reduced selection e ciency. In such situations where none of the above mass limits can apply, the generic lower limit of approximately 45 GeV, derived from the analysis of the Z-width, is still valid since this is independent of the eld composition and of the decay modes of the charginos. Note that unlike neutralinos which couple to the Z-boson only via

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e[notdef]0i

m[tildewide][notdef]

m[tildewide]

01 or m = m[tildewide][notdef]

1 > 92.4 GeV for degeneracy in the higgsino region ([notdef][notdef][notdef] [notdef]M1[notdef], [notdef]M2[notdef]) [13, 14]. Without assuming gaugino mass unication,

a lower limit of m[tildewide][notdef]

1 > 70 GeV was set for any m+ and m[tildewide]

their higgsino component, the charginos couple to Z via both their gaugino as well as higgsino components; so it is not possible to avoid the Z-width constraint for a light chargino.

Sneutrino. Light sneutrinos can only decay invisibly to

e[notdef]01 unless the decays to charginos and heavier neutralinos are not kinematically suppressed. The invisible width of the Z-boson puts a lower limit on the left-sneutrino mass of 43.7 GeV, which improves slightly to 44.7 GeV if all three sneutrinos are mass-degenerate. Note that the lightest left-sneutrino by itself cannot be a cold DM candidate [86, 87], and we must introduce a mixing with a SM singlet sneutrino to make it a viable DM candidate (see, e.g., [88 94]). Since we are dealing here only with the MSSM eld content and do not have a right-sneutrino component, we discard those points for which the sneutrino is the LSP.

Slepton. Studies of the Z-boson width and decays put a lower bound on the slepton masses m[tildewide][lscript]R(L)

ee,

quoted for

e[notdef]01 .

For smuons and staus, the LEP limits are independent of the MSSM parameters [95], and hence, directly applicable to our case. However, the selectron mass limit will be di erent if we do not assume gaugino mass unication due to a di erent production cross section involving the t-channel neutralino exchange, in addition to the usual s-channel /Z exchange. Since there is no dedicated analysis of the LEP data addressing this issue available in the literature and this is beyond the scope of our present work, we only use the generic lower bound for

ee derived from the Z-width in our numerical analysis, but will also comment on the implications of the tighter selectron mass bound from LEP on our light neutralino scenario. We will also include the latest 95% C.L. LHC exclusion limits for slepton pair production interpreted in the slepton-neutralino mass plane of pMSSM [96] which are applicable to both left- and right-handed selectrons and smuons.

Gluino and squarks. The current LEP limits on the squark masses are similar to the slepton mass limits of O(100) GeV. However, since squarks are colored objects, their

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> 40 (41) GeV, independently of the decay modes for individual sleptons (

e[lscript] =

e). This limit improves to 43 GeV if all the three slepton avors are mass-degenerate. Tighter limits can be obtained assuming that sleptons are pair-produced at LEP, and each slepton dominantly decays to [lscript]

e[notdef]01, thus leading to two back-to-back leptons and missing transverse momentum. These limits are valid for a mass splitting m[lscript] = m[tildewide][lscript]

m[tildewide][notdef]01 >

15 GeV so that the nal state leptons are not too soft. Moreover, the LEP results are interpreted assuming that only

e[lscript]R e[lscript]R production contributes, and hence, the limits are usually

e[notdef],

e[lscript]R, since it is typically lighter than e[lscript]L in most SUSY models, and has a weaker coupling to the Z-boson so that the limits are more conservative. This is a good approximation for selectrons and smuons, but not for staus which can have signicant mixing between the avor eigenstates

eL and eR. The most conservative limit on the mass of the lightest stau is obtained with a mixing angle [tildewide]

[similarequal] 52 which minimizes the production cross section.

The slepton mass limits of O(100) GeV quoted in ref. [13, 14] were derived under

the assumption of gaugino mass unication at the GUT scale which was used to x the masses and composition of neutralinos. It was also assumed that the slepton branching ratio to [lscript]

e[notdef]01 is nearly 100% which is a good approximation if the second lightest neutralino is heavy enough to suppress the cascade decay into [lscript]

e[notdef]02 followed by e[notdef]02 ! f

e[notdef]01 or

production cross sections are much higher at hadron colliders. The highest sensitivity on squark and gluino production now comes from the LHC experiments. The generic lower limit on the rst/second generation squark masses is 600750 GeV and on the gluino mass is 700900 GeV, as set for simplied SUSY models by the ATLAS analysis of the 8 TeV LHC data [26]. The corresponding CMS limits are very similar [27]. However, from the latest global t of pMSSM after the LHC results [60] (see also ref. [97, 98] for an earlier global t of pMSSM), the corresponding lower limit on squark mass is m[tildewide]q

hence, we use this value to constrain our pMSSM parameter space.

The LHC and Tevatron limits on the third generation squarks are usually weaker since the amount of bottom and top quark content in the proton is negligible, and hence, the direct production of bottom and top squark is suppressed with respect to the rst/second generation squarks. The current exclusion limit for top squarks is between 300600 GeV from the LHC data, depending on the decay channel [26, 27]. Similar limits have been derived for the bottom squark as well. Following the latest global t of pMSSM [60], we set the lower limits for light top squark and sbottom masses at 400 GeV and 300 GeV, respectively. Note that these limits are applicable as long as the light stop/sbottom is not highly mass degenerate with the lightest neutralino (with m < 10 GeV or so) which always turns out to be the case for our light neutralino solutions satisfying all the other constraints. Thus we do not have any light sbottom solutions as considered in ref. [39].

The lower limits on the sparticle masses derived from the above discussion are summarized in table 2. We emphasize here that for a light neutralino DM with m[tildewide][notdef]

01 < mZ/2 as

considered in our case, the dominant annihilation channels will be the t-channel processes mediated by light sfermions unless the s-channel Z-resonance or co-annihilation are e ective. Hence, the lower limits on the chargino and sfermion masses as given in table 2 are crucial ingredients in our numerical analysis.

Bs ! +

The rare decay Bs ! [notdef]+[notdef] is known to be a sensitive channel for new physics since its

SM predicted rate is small due to helicity suppression. Recently, the rst evidence for this decay was observed by the LHCb collaboration with the measured branching ratio: B(Bs !

[notdef]+[notdef]) = 3.2+1.51.2

[parenrightbig]

[notdef] 109 [24] which is in excellent agreement with the SM prediction of

(3.23 [notdef] 0.27) [notdef] 109 [25], thus raising some concerns for the health of SUSY. However, it

must be noted that the upper limit derived from the latest LHCb result is actually slightly weaker than the earlier upper limit of < 4.5 [notdef] 109 [99]. The e ect of the new results is

mostly felt in the large tan > 50 regions of the MSSM parameter space [100] which are also strongly constrained from direct SUSY searches and the MSSM Higgs searches.

b ! s

We have also included the constraint from the radiative B-meson decay branching ratio,

B(b ! s ) = (3.55 [notdef] 0.24 [notdef] 0.09) [notdef] 104 [101] which is somewhat higher than the SM

prediction of (3.15 [notdef] 0.23) [notdef] 104 [102]. Thus large SUSY corrections are preferred which

mainly occur for light chargino and top squarks and for large tan [103].

[greaterorsimilar] 500 GeV, and

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Particle Mass limit (GeV) Validity Condition

e[notdef][notdef]1 103.5 m[tildewide][notdef]+1 m[tildewide][notdef]01 > 3 GeV, m

45 generic LEP bound

e[notdef]R 88 m[tildewide][notdef]R m[tildewide][notdef]01 > 15 GeV, BR(

e1 76 m[tildewide]1 m[tildewide][notdef]01 > 15 GeV, BR(

eeR 95 m[tildewide]eR m[tildewide][notdef]01 > 15 GeV, BR(

ef > m[tildewide][notdef]

70 m[tildewide]

> 300 GeV, [notdef][notdef][notdef] [notdef]M2[notdef]

e1 !

e[notdef]01) = 1, [notdef] = 200 GeV, tan = 2

e[lscript]R (L) 40 (41) generic LEP bound

e 43.7 generic LEP bound

eg 800

eq 500

et1 400

eb1 300

Table 2. The lower limits on the sparticle masses used in our numerical analysis. The chargino and slepton mass limits are derived from the LEP data [13, 14] while the squark and gluino mass limits are derived from the LHC data [26, 27] which now supersede the LEP as well as the Tevatron [69, 70] limits.

(g 2)

Another important constraint comes from the muon anomalous magnetic moment a[notdef] (g

2)[notdef]/2 which gives a more than 3 discrepancy with the SM prediction: a[notdef] = (26.1[notdef]8.0)[notdef]

1010 [104]. The SUSY contribution to a[notdef] can explain this discrepancy with relatively light smuons and/or large tan [105107], and [notdef] < 0 region of the SUSY parameter space is strongly disfavored (unless the electroweak gaugino masses M1, M2 < 0).

Higgs sector

For the light CP -even Higgs mass, we have chosen the value of mh = (125 [notdef] 2) GeV,

following the latest best-t mass measurements of the Higgs-like particle discovered at the LHC: (125.2 [notdef] 0.3 [notdef] 0.6) GeV (ATLAS) [108] and (125.8 [notdef] 0.4 [notdef] 0.4) GeV (CMS) [109].

For the other MSSM Higgs bosons, we ensure that all our allowed points satisfy the latest LHC constraints on the mA tan plane [110, 111] and on the MSSM charged Higgs

mass [112, 113] which are related to each other at tree-level by m2H = m2A + m2W . Note that the non-decoupling region with light mA 95 130 GeV, almost mass-degenerate

with the light CP -even Higgs, and with the heavy CP -even Higgs SM-like, is disfavored [114, 115] by the latest LHC Higgs data and avor constraints, especially the Bs ! [notdef]+[notdef] and b ! s . Hence, we work in the decoupling region with mA > 300 GeV

with the light CP -even Higgs SM-like with mass in the vicinity of 125 GeV, and with the heavy CP -even Higgs nearly mass-degenerate with the CP -odd Higgs. Also note that for

e[notdef] ! [notdef]

e[notdef]01) = 1

ee ! e

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e[notdef]01 coupling is small enough to satisfy the current global limit on the Higgs invisible decay branching ratio: BRinv < 0.28 at 95% CL [116].

Dark matter constraints

The latest results from Planck give the current relic density of the cold dark matter content in our universe to be [notdef]h2 = 0.1199 [notdef] 0.0027 at 68% CL [72]. The corresponding

value from the 9-year WMAP data is [notdef]h2 = 0.1148 [notdef] 0.0019 [71]. For the relic density of

the neutralino DM in our case, we only require it to satisfy the WMAP 2 upper bound combined with 10% theoretical uncertainty: [tildewide][notdef]

a mostly bino-like neutralino, the h

e[notdef]01

01 h2 < 0.138 which also encompasses the latest observed value from Planck. The cases where the neutralino relic density is below the corresponding WMAP lower bound, [tildewide][notdef]

01 h2 < 0.091, could account for the correct relic density by alternative mechanisms of regeneration (see e.g., [117119]), or by invoking a multi-component DM scenario (see e.g., [120129]).

As far as the DM direct detection constraints are concerned, since there is no unanimous upper bound on the direct detection cross section, we do not put this constraint a priori on the model parameter space. However, as we will see later, most of the allowed parameter space satisfying the other constraints also satisfy the most stringent upper limit on the spin-independent DM-nucleon scattering cross section set by the XENON100 experiment [10]. Note that for m[notdef] > 10 GeV, the spin-independent direct detection constraints are more stringent than the collider constraints from mono-jet [130, 131] and isolated mono-photon [132, 133] searches at the LHC as well as from the LEP mono-photon data [134].

Complementary to the direct detection constraints, there exist indirect detection constraints which are mostly sensitive to light WIMPs annihilating to SM fermions which eventually lead to gamma-ray signals. A lower limit of m[tildewide][notdef]

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01 [greaterorsimilar] 10 GeV was derived from the CMB constraints [135140]3 for DM candidates with a velocity-independent annihilation cross section of [angbracketleft]av[angbracketright] = 3 [notdef] 1026cm3 [notdef] s1. Under the same assumption, the Fermi-LAT

data put lower bounds of m[tildewide][notdef]

01 [greaterorsimilar] 27 GeV for annihilation to bb channel and m[tildewide][notdef]

01 [greaterorsimilar] 37 GeV

for + channel [142]. However, these bounds can be relaxed if we include the velocity-dependent contributions, as shown for pMSSM in ref. [143]. In our numerical analysis, we include the latest Fermi-LAT 95% CL upper limit on the integrated -ray ux from spectral line searches in the Milky Way galaxy: < 4 [notdef] 1010cm2 [notdef] s1 [73] for high latitude

([notdef]b[notdef] > 10 ) plus a 20 [notdef] 20 square at the galactic center and for 7200 GeV energy range.

The various experimental constraints discussed above and used in our numerical analysis, in addition to the sparticle mass limits listed in table 2, are summarized in table 3.

4 Results

In order to scan the 19-dimensional pMSSM parameter space more e ciently while satisfying all the constraints listed in tables 2 and 3, we have performed a MCMC analysis using a Gaussian distribution of likelihood function: f(x, x0, ) = exp[(x x0)2/22] for

3Similar limits have also been derived from BBN constraints [141].

Parameter Constraint mh (125 [notdef] 2) GeV

invisibleZ < 3 MeV [tildewide][notdef]

01 h2 < 0.138 < 4 [notdef] 1010 cm2 [notdef] s1

B(Bs ! [notdef]+[notdef]) 3.2+1.51.2

[parenrightbig]

[notdef] 109

B(b ! s ) (3.55 [notdef] 0.26) [notdef] 104

a[notdef] (26.1 [notdef] 8.0) [notdef] 1010

Table 3. The relevant experimental constraints used in our analysis, in addition to those listed in table 2.

all the observables, with a preferred value x0 [notdef] . We have used CaclHEP2.3 [144] and

micrOMEGAs2.4 [145147] to compute all the observables, together with SoftSUSY [148] for calculating the particle spectrum.

First we discuss our MCMC scan results for the relic density of a light neutralino DM candidate as shown in gure 1, which was obtained by numerically solving the Boltzmann equation using micrOMEGAS [145]. We require all the allowed points (shown as circles) to satisfy the experimental constraints given in table 3, along with the LEP limits on sparticle masses given in table 2. The latest LHC results put much tighter bounds on the strongly interacting squarks and gluinos and further eliminate some of these otherwise allowed parameter space, as shown by the starred points in gure 1. The WMAP-9 2 band is shown in grey, whereas the latest Planck result is shown as dark shaded region. We nd that light neutralinos with mass as low as 10 GeV are still allowed, though severely ne-tuned with the electroweak ne-tuning measure dened by eq. (2.4): tot 1. This can be understood as follows by analyzing the gaugino and higgsino components of the lightest neutralino as well as its dominant annihilation channels.

The bino, wino and higgsino fractions of the lightest neutralino for all the allowed points in our pMSSM parameter space are shown in gure 2. We reproduce the well-known result that the lightest neutralino is mostly bino-like for masses below mZ/2, mainly due to the invisible Z-decay width constraint in eq. (3.4). However, a purely bino DM tends to overclose the universe unless it has an e cient annihilation channel to reach up to the thermal WIMP annihilation rate of 3 [notdef] 1026 cm3 [notdef] s1. One possibility is to consider

a well-tempered neutralino [149] which corresponds to the boundary between a pure bino and a pure higgsino or wino. Another possibility to reduce the bino relic density is by annihilation via the t-channel slepton exchange (the so-called bulk region) which is e cient for light sleptons, or by using co-annihilation with a light slepton, squark, chargino or second-lightest neutralino in congurations where such light sparticles are not yet excluded by experimental searches. We nd that most of the points with m[tildewide][notdef]

01 close

to 45 GeV can have either slepton co-annihilation or a resonant Z-annihilation due to a non-negligible higgsino component, and hence, can easily satisfy the WMAP upper limit

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Figure 1. The relic density of a light neutralino DM in pMSSM satisfying all the experimental constraints discussed in section 3. The color-coding denotes the ne-tuning measure dened by eq. (2.4). The points denoted by circles satisfy all the experimental constraints, except that the squark masses are only required to satisfy the LEP lower limits. For the starred points (a subset of the circled points), the corresponding squark masses satisfy the latest LHC constraints. The top (bottom) grey horizontal line shows the 2 upper (lower) limit of the cold dark matter relic density from WMAP-9 data, whereas the black (shaded) region shows the 1 allowed range from the recent Planck data.

Figure 2. The gaugino (

our pMSSM parameter scan.

on the relic density. These points are also less ne-tuned. On the other hand, the light neutralino DM points in the 1030 GeV range as shown in gure 1 have to be mostly bino-like and lie in the bulk region, thus leading to signicant ne-tuning. Note that in the latter case, the next-to-lightest supersymmetric particle (NLSP) masses are much higher than the LSP mass, thus eliminating the possibility of a co-annihilation.

This is further claried in gure 3 where we show the various NLSPs and their masses as a function of the lightest neutralino mass. We see that all the allowed points

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eB,

fW 0) and higgsino (

eH0d,

eH0u) components of the lightest neutralino in

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Figure 3. The various NLSP masses as a function of the LSP mass for the allowed points (circles) shown in gure 1. The LEP exclusion regions strictly applicable for

e[notdef]R (red shaded) and e1 (green

e[lscript] (l = e, [notdef]) (blue shaded) are also shown.

01 < 30 GeV have a charged slepton NLSP with mass below 100 GeV. Especially the points with a light stau are severely ne-tuned since they usually require a mass suppression by the o -diagonal elements in the slepton mass matrix, or a large [notdef]-term. We also show in gure 3 the LEP exclusion regions in the charged slepton-neutralino mass plane, derived under the assumption of gaugino mass unication [13, 14]. The limits for light smuons and staus are still applicable to the pMSSM case as long as m[lscript] > 15 GeV,

but not directly to light selectrons if we assume non-universal gaugino masses, and hence, can still allow the low neutralino mass regime. The latest 95% C.L. ATLAS exclusion limits [96] are also shown in gure 3 which were derived from searches for direct slepton (selectron and smuon) pair production and interpreted in the pMSSM. A similar dedicated analysis of the LEP data is required in order to completely rule out the light selectrons, and hence, the lightest neutralino DM mass below 30 GeV for the pMSSM scenario.

The neutralino DM-nucleon spin-independent scattering cross-sections for the allowed points is shown in gure 4. The points corresponding to the observed relic density within the WMAP band in gure 1 are encircled. As mentioned earlier, the remaining points can also account for the correct relic density if we assume 100% regeneration at late times (see e.g., [117119]). Another possibility is to invoke a multiple DM scenario (see e.g., [120 129]) in which case the neutralino DM considered here will only constitute a fraction of the total observed DM density, and we must scale the neutralino DM density appropriately in order to calculate the neutralino-nucleon scattering cross section. Since the cross section depends linearly on the DM density, we use a rescaling factor of r[notdef] [tildewide][notdef]

with m[tildewide][notdef]

shaded) and the LHC exclusion region for

01 / observed, where for concreteness, we take the Planck central value for observedh2 = 0.12. For the DM

density distribution in the galactic halo, we have used the NFW prole [150, 151], as implemented in micrOMEGAs 2.4 [146]. The results with and without rescaling of the DM density are shown for comparison in gure 4. A comparison of the two panels in gure 4 shows that the light neutralino solutions (with large ne-tuning) are mostly una ected by

Figure 4. The spin-independent direct detection cross-section values for the allowed points in our pMSSM scan. The color-coding and labeling of the points are same as in gure 1. The circled points correspond to those within the WMAP allowed band in gure 1. The left (right) panel shows the cross section without (with) rescaling of the DM density. The current upper limit from the XENON100 experiment and the projected limits from LUX and XENON1T experiments are shown as solid lines. The 2-preferred range of CRESST-II is shown as the shaded region.

the rescaling since these points yield a relic density value more than 10% of the observed value (see gure 1). It is interesting to note that most of the allowed region in gure 1 with low ne-tuning lead to a higher scattering cross section via Z-boson exchange and are already ruled out, even after rescaling, by the latest XENON100 data [10] or will be ruled out by the projected limit of XENON1T experiment [74] (and also LUX [75]) if they still get a null result. The points which survive with rescaling must be part of some multi-component DM scenario. In the light of the recent claims for positive hints of a light DM from some experiments, it is worth mentioning here that a few of our solutions with SI 107 pb are in the vicinity of the 2 preferred range of the CRESST-II results [9],

but not compatible with the favored regions of DAMA [6, 7] or CoGeNT [8].

Figure 5 shows the integrated photon ux from spectral lines due to neutralino DM annihilation in the galactic halo. We have assumed the NFW prole for the DM density distribution, as implemented in micrOMEGAs 2.4 [147]. We do not consider galactic sub-structures or clumpy DM congurations since a proper analysis of these e ects would require a detailed numerical simulation well beyond the scope of this work. As in gure 4 for scattering cross-section, we have shown the uxes for both the cases without and with scaling of the neutralino DM density. In the latter case, we have used the scaling factor r2[notdef] for the thermally-averaged annihilation cross section [angbracketleft]av[angbracketright] when the neutralino

DM relic density is below the observed value. The light neutralino solutions with a relic density more than 10% of the observed value (cf. gure 1) are mostly una ected by the rescaling. Note that since the LSP in our case is mostly bino-like with heavy squarks and higgsinos and the charginos are not mass-degenerate with the LSP, the annihilation to photons is loop-suppressed, and hence, the photon line emission will be small. It is clear from gure 5 that the current sensitivity of Fermi-LAT [142] still leaves all of our allowed parameter space untouched. The future data from ongoing Fermi-LAT and next generation gamma-ray searches might be able to probe our allowed parameter space with a photon line signal [152].

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Figure 5. The integrated photon ux from annihilation of the neutralino DM as a function of its mass. The color-coding and labeling of the points are same as in gure 4. The solid horizontal line shows the current upper limit from the Fermi-LAT data.

Figure 6. The allowed parameter space for some of the relevant pMSSM parameters consistent with a light neutralino DM. The color-coding and labeling of the points are the same as in gure 1.

For completeness, we also show in gure 6 some other relevant pMSSM parameters with respect to the lightest neutralino mass. The mA tan parameter space is mostly

consistent with the latest MSSM Higgs sector limits from the LHC [110, 111]. As for the bino mass parameter M1, it is clear that a relatively small value of [notdef]M1[notdef] < 100 GeV is

preferred to obtain a light bino-like neutralino LSP. Finally, as is well-known, a relatively large value of [notdef]At[notdef] is required in order to enhance the radiative corrections for the light

CP -even Higgs mass to be consistent with the LHC-preferred value of 125 [notdef] 2 GeV.

Finally, we wish to point out that the allowed sparticle spectra discussed here with mostly heavy squarks, and with light sleptons, chargino and bino-like neutralino LSP, are

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also crucial for explaining the muon (g2) anomaly [153], while simultaneously satisfying all

the other experimental constraints. Light staus with sizable left-right mixing can also lead to an enhanced h ! decay rate [154156], which might be able to explain the persistent

excess in the Higgs signal strength in this channel: 1.65 [notdef] 0.24(stat)+0.250.18(syst) [157].

5 Conclusion

We have studied the naturalness of a light neutralino dark matter candidate in the MSSM in the light of the latest results from the collider (LEP, Tevatron and LHC), avor (LHCb) and dark matter (XENON100, WMAP-9, Planck) sectors. In particular, keeping in mind the recent positive hints for a light DM below 45 GeV in some direct detection experiments and the null results from SUSY searches at the LHC, we perform a dedicated study focusing on the possibility of a light DM candidate in the form of the lightest neutralino in the pMSSM, also analyzing the naturalness of such a scenario. We include all the new results from the ongoing LHC experiments in our analysis, such as the null results from the SUSY searches, the observation of a Higgs-like particle, the observation of the rare meson decay Bs ! [notdef]+[notdef], and the updated constraints on the MSSM Higgs sector. We

also take into account the 9-year WMAP results as well as the recently released Planck results for the DM relic density and the Fermi-LAT data for the integrated photon ux. In order to e ciently scan over the 19-dimensional pMSSM parameter space, we perform a MCMC likelihood analysis focusing on a light neutralino with mass below the LEP bound of 46 GeV (applicable to gaugino mass unication models).

We nd that a light neutralino DM with mass as low as 10 GeV is still allowed in the pMSSM, while satisfying all the existing experimental constraints. However, such neutralinos which are required to be mostly bino-like are severely ne-tuned and require the existence of light sleptons with mass below 100 GeV in order to provide an e cient annihilation channel to reduce the DM relic density below the observed upper limit. Such light smuons and staus are excluded from LEP searches while light selectrons are excluded only if we assume gaugino mass unication. A dedicated analysis of the LEP data in the context of a pMSSM scenario could completely eliminate the possibility of a light neutralino DM in the mass range of 1030 GeV. We also nd that for the allowed parameter space, other possible solutions in this mass range as discussed in the literature (e.g., light sbottom NLSP) are now excluded mainly due to the latest LHC results on the strongly interacting sfermion sector.

On the other hand, low ne-tuning regions can be obtained around m[tildewide][notdef]

01 = 45 GeV

where the resonant annihilation via the s-channel Z-exchange is possible for a bino-higgsino mixture of neutralino LSP. However, such regions also predict a higher spin-independent DM-nucleon scattering cross section, and are mostly excluded by the recent XENON100 limits. The remaining such points are within the reach of the XENON1T projected limits.

In conclusion, while a light neutralino DM with mass below 46 GeV has been conclusively ruled out in MSSM with gaugino mass unication by LEP searches, such a possibility in a general version of MSSM is of enormous interest in the light of the recent claims for a positive signal in some DM direct detection experiments. Taking into account the latest experimental results from collider, avor, dark matter and

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astrophysical/cosmological sectors, we show that such a light neutralino DM scenario is also getting highly constrained in MSSM without gaugino mass unication. However, within a pMSSM scenario, there still exists some parameter space for light neutralino DM which could be completely probed by a dedicated analysis of the existing experimental data, in combination with the ongoing searches.

Note added. After the submission of our paper, another DM direct detection experiment, namely, CDMS-II [158], has reported three WIMP-candidate events with an expected background of 0.7 events. Their best-t WIMP mass is 8.6 GeV with the WIMP-nucleon cross section of 1.9 [notdef] 105 pb. This bolsters our motivation in this work to examine the

allowed parameter space for a light neutralino DM candidate in the MSSM.

Acknowledgments

We thank Matthew Dolan and Patrick Janot for valuable discussions and comments on the draft, and Jonathan Da Silva for useful discussions regarding the MCMC analysis. CB is supported by the ERC advanced grant DARK at IAP, Paris. The work of PSBD and AM is supported by the Lancaster-Manchester-She eld Consortium for Fundamental Physics under STFC grant ST/J000418/1. EP is supported by STFC ST/J501074.

Open Access. This article is distributed under the terms of the Creative Commons Attribution License which permits any use, distribution and reproduction in any medium, provided the original author(s) and source are credited.

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JHEP06(2013)113

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SISSA, Trieste, Italy 2013

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We examine the possibility of a light (below 46 GeV) neutralino dark matter (DM) candidate within the 19-parameter phenomenological Minimal Supersymmetric Standard Model (pMSSM) in the light of various recent experimental results, especially from the LHC, XENON100, and Planck. We also study the extent of electroweak fine-tuning for such a light neutralino scenario in view of the null results from the searches for supersymmetry so far. Using a Markov Chain Monte Carlo likelihood analysis of the full pMSSM parameter space, we find that a neutralino DM with mass 10 GeV can in principle still satisfy all the existing constraints. Our light neutralino solutions can be broadly divided into two regions: (i) The solutions in the 10-30 GeV neutralino mass range are highly fine-tuned and require the existence of light selectrons (below 100 GeV) in order to satisfy the observed DM relic density. We note that these are not yet conclusively ruled out by the existing LEP/LHC results, and a dedicated analysis valid for a non-unified gaugino mass spectrum is required to exclude this possibility. (ii) The solutions with low fine-tuning are mainly in the 30-46 GeV neutralino mass range. However, a major portion of it is already ruled out by the latest XENON100 upper limits on its spin-independent direct detection cross section, and the rest of the allowed points are within the XENON1T projected limit. Thus, we show that the allowed MSSM parameter space for a light neutralino DM below the LEP limit of 46 GeV, possible in supersymmetric models without gaugino mass unification, could be completely accessible in near future. This might be useful in view of the recent claims for positive hints of a DM signal in some direct detection experiments.

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Title

Naturalness of light neutralino dark matter in pMSSM after LHC, XENON100 and Planck data

Author

Boehm, Céline; Bhupal Dev, P S; Mazumdar, Anupam; Pukartas, Ernestas

Pages

1-29

Publication year

2013

Publication date

Jun 2013

Publisher

Springer Nature B.V.

e-ISSN

10298479

Source type

Scholarly Journal

Language of publication

English

DOI

https://doi.org/10.1007/JHEP06(2013)113

ProQuest document ID

1652921141

SISSA, Trieste, Italy 2013

Naturalness of light neutralino dark matter in pMSSM after LHC, XENON100 and Planck data

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