text:
\section{Introduction}

N=1 supersymmetry broken around the weak scale would be the prime new
physics candidate to be searched at the LHC. It provides not only an
appealing explanation for the origin of the electroweak symmetry
breaking but also a natural dark matter (DM) particle of the
Universe. While N=1 supersymmetry is enforced by the chiral structure
of matter fields in the Standard Model, the gauge sector may be
extended to have N=2 supersymmetry in which gauginos can be Dirac
particles
\cite{hall91,Randall92,fox02,nelson02,fox04,benakli05,benakli06,
  benakli08,amigo08} (for a review of N=2 supersymmetry, see
\cite{N=2}). Determining the Majorana/Dirac nature of gauginos
will be an interesting task for future experiments looking for
supersymmetric CP and flavor violation~\cite{hisano06,kribs07},
collider signatures \cite{nojiri07,drees08}, and dark matter
properties~\cite{ullio06,hsieh07,kribs08,benakli09}.

There are some important distinctions between Majorana and Dirac
gauginos. First, the annihilation of a Dirac gaugino pair into a
fermion--antifermion pair, $\chi\bar{\chi} \to f\bar{f}$, has a
non-vanishing $s$--wave contribution even in the limit of vanishing
fermion masses, and thus the leptonic final states are not
suppressed. This implies that a Dirac gaugino can provide a viable DM
explanation for the abundance of energetic electrons and positrons
recently observed in cosmic
rays~\cite{HEAT,AMS-01,PAMELA,PPB-BETS,ATIC,HESS,FERMI}. Second, Dirac
gauginos can have a vector coupling with the $Z$ gauge boson,
$\bar{\chi}\gamma_\mu\chi\, Z^\mu$, leading to sizable
spin--independent scattering off nuclei.  As a consequence, the
Higgsino component in the DM gets constrained by the direct detection
data \cite{CDMS} and also by the non-observation of antiproton
excesses in PAMELA \cite{pbar} as will be discussed in detail in the
following.

In order to ensure such Dirac nature of DM, Majorana mass terms,
which provide the mass splitting between the Dirac components,
have to be highly suppressed. Otherwise, the heavier component of
the two quasi-degenerate Majorana gauginos will decay to the
lighter one, and the galactic DM will consist of a pure Majorana
gaugino.  If one assumes the N=2 structure in the Higgs sector,
i.e. that the two Higgses $H_u$ and $H_d$ form an N=2
hypermultiplet \cite{benakli06,benakli08}, the Dirac structure
imposed at the tree level is spoiled by a large amount due to
radiative corrections with Higgs--Higgsino and fermion--sfermion
in the loop.  A way to enforce an (almost) pure Dirac property for
gauginos is then to assume a continuous R symmetry which forbids
the usual $\mu$ term for the Higgs bilinear coupling $H_u H_d$ and
the soft breaking trilinear $A$ term~\cite{kribs07}.

In this paper, we will work out a framework for R--symmetric Dirac
gauginos, which are introduced by extending the gauge/Higgs sector
of a supersymmetric model. We assume the Dirac bino as the main
component of the lightest supersymmetric particle. The
annihilation of two Dirac binos into a lepton--antilepton pair
usually dominates over the annihilation into a quark--antiquark
pair, as sleptons are typically much lighter than squarks. As we
will see, the annihilation to a CP even final or intermediate
state turns out to be velocity--suppressed, which is a property
that is also true in the usual Majorana gaugino case.  Then, the
Dirac bino annihilation to the two $W$ bosons ($W^+W^-$) and that
to a CP even Higgs boson and a $Z$ boson ($hZ$), both controlled
by the Higgsino component in the DM particle, turn out to be the
next important sources of the cosmic antiproton flux.  Quantifying
the suppression factor for the Higgsino component, one can make a
prediction for the direct detection rate.

In Section 2, an R--symmetric N=2 extension of the Minimal
Supersymmetric Standard Model is introduced to enforce an almost pure
Dirac gaugino structure. Based on this framework, we derive
interaction vertices for the Dirac bino, which is assumed to be the
dark matter, and then provide a qualitative analysis for its indirect
and direct detection properties in Section 3. A numerical analysis is
performed in Section 4 to obtain various fits and constraints of the
leptophilic Dirac bino dark matter from the current indirect and
direct detection data. We give our conclusions in Section 5.

\section{The R--symmetric gauge/Higgs sector and Dirac bino couplings}
\label{sec:r_symmetric}

Let us first note that a small Majorana mass term, breaking the
Dirac structure,  will produce quasi-degenerate two Majorana
gauginos,  the heavier of which will then decay to the lighter
one.  Assuming a tiny splitting $\delta m_M$ in the Dirac bino
components, one expects to have one--loop diagrams generating the
magnetic moment operator:
\begin{equation}
    {\alpha' \over 4\pi} { m_{\tilde{B}} \over \tilde{m}^2}
    \tilde{B}_1 \Sigma_{\mu\nu} \tilde{B}_2 F^{\mu\nu}\,,
\end{equation}
between two almost degenerate Majorana components
($m_{\tilde{B}_2} - m_{\tilde{B}_1} = \delta m_M$) where
$m_{\tilde{B}}\approx m_{\tilde{B}_{1,2}}$  is the almost
degenerate bino mass and $\tilde{m}$ is a sfermion mass. The decay
rate for the process $\tilde{B}_2 \to \tilde{B}_1 \gamma$ is
\begin{equation}
 \Gamma \approx {\alpha\over 4\pi} \left( {\alpha'\over 4\pi}
 {m_{\tilde{B}}^2 \over \tilde{m}^2} \right)^2 \delta m_M \,.
\end{equation}
In order to maintain the Dirac gaugino structure for the present
DM, we require that its lifetime is larger than the age of the
Universe. This gives us
\begin{equation} \label{deltamM}
 \delta m_M \lesssim 10^{-33}\, \mbox{GeV}\,,
\end{equation}
for $m_{\tilde{B}} \sim \tilde{m}$.  Thus, the Majorana gaugino
mass term has to be suppressed below the order of $\delta m_M \ll
m_{3/2}^3/M_P^2$, where $m_{3/2}$ is the gravitino mass $\sim 1$
TeV. In N=1 supergravity, a nonzero value of the superpotential
$w_0$ is required to tune the cosmological constant.  As $w_0$
breaks an R symmetry, it can usually generate Majorana gaugino
masses of the order of $m_{3/2} \sim w_0$.  In fact, avoiding such
a leading contribution to gaugino masses and $A$ or $B$  soft
supersymmetry breaking terms has been discussed in the context of
split supersymmetry \cite{arkani04}. Furthermore, a loop
contribution from anomaly mediation was also shown to be further
suppressed \cite{arkani04,luty02}.  Concerning the anomaly
mediation contribution,  it is interesting to remark that,
saturating the lower bound, one finds  $\delta m_M \sim
(g^2/16\pi^2)(1/16\pi^2)(m_{3/2}^3/M_P^2)$ \cite{arkani04} which
can be compatible with the condition (\ref{deltamM}).

An almost R--symmetric supersymmetry breaking can be realized in the
following way. Let us introduce an extended gauge--Higgs sector
\cite{kribs07}:
\begin{equation}
    W'
   = \mu_1 H_d R_u + \mu_2 R_d H_u
   - \sqrt{2} g_a (\xi_1 H_d T^a R_u\,
    + \xi_2 H_u T^a R_d)\, \Phi^a \,,
\label{newgauge}
\end{equation}
where $\Phi^a= (\phi^a, \psi^a)$ is the N=2 counterpart of the gauge
superfield $W^a_\alpha$.  In our phenomenological approach, the N=2
structure is supposed to be broken in an appropriate way leading to an
effective N=1 superpotential, as discussed below.
For instance, $\xi_{1,2}$ in Eq.~(\ref{newgauge}) are arbitrary
parameters breaking the N=2 relation. Note that the usual Higgs
superfields $H_{d,u}$ cannot form an N=2 hypermultiplet as the
corresponding $\mu$ and $B$ terms, breaking an R symmetry, will
generate a large Majorana mass $m_{1/2} \propto (\alpha/4\pi) \mu
B$ at one--loop. A similar one--loop contribution arises also from
the presence of left--right mixing sfermion masses, depending on
the $\mu$ or $A$ term. Thus, we are forced to extend the Higgs
sector to avoid the usual $\mu$ and $B$ terms and we will consider
a situation in which the N=2 structure is not respected in the
extended Higgs sector. Now let us introduce a supersymmetry
breaking field $X$ and two R symmetries, denoted by ${\cal R}$ and
${\cal J}$, which are broken by two order parameters $x_0$ and
$w_0$.  The R charge assignment is given by
\begin{equation}
 \begin{array}{c|ccccccc}
 & W^a_\alpha & \Phi^a & H_{d,u} & R_{u,d} & X & x_0 & w_0 \cr
 \hline
{\cal R} &  1 & 2 & 0 & 0 & 0 & 2 & 2 \cr {\cal J} & 1 & 0 & -1 &
3 & 2 & 0 & 2 \cr
\end{array}\;.
\end{equation}
Note that the two R symmetries are not compatible with the N=2
structure \cite{N=2} as different ${\cal J}$ charges are assigned
to $H_{d,u}$ and $R_{u,d}$ and thus they are not considered to
come from the same hypermultiplets.  The superpotential of the
supersymmetry breaking sector can be written as
\begin{equation}
 W = w_0 + x_0 X\,,
\end{equation}
which gives $\langle X \rangle = \theta^2 F_X$, where $F_X=x_0 \sim
m_{3/2} \sim w_0$ is assumed.  Now one can see that the Dirac
gaugino mass and the extended $\mu$ terms can come from the
following F or D terms:
\begin{equation} \label{eqFD}
 X W^a_\alpha Q_\alpha \Phi^a\big|_F
 \,,\quad H R \Phi\big|_F\;\;\mbox{or}\;\; HRX^\dagger\big|_D\;,
\end{equation}
where $Q_\alpha$ is the supersymmetric covariant derivative. The
last two terms in the above equation reproduce the superpotential
(\ref{newgauge}) and the first term gives the Dirac gaugino mass
term: ${\cal L}_{soft} = M_a \psi^a \tilde{W}^a$. In the
following, we will concentrate on the Dirac gauginos in the
electroweak sector.  The Dirac bino (wino) mass is denoted by
$M_1$ ($M_2$).
The Majorana gaugino mass (and similarly the $A$ term) gets a
contribution from
\begin{equation}
  W^a_\alpha W^a_\alpha W_0^\dagger X X^\dagger\big|_D \,.

\end{equation}
This gives the (Majorana) soft term
${\cal L}_{soft} = \delta m_M \tilde{W}^a \tilde{W}^a$ with
 $\delta m_M \sim  m_{3/2}^3/M_P^2$ which can be
compatible with the bound (\ref{deltamM}) assuming a small
coefficient of the order of $10^{-4}$ for $m_{3/2}\sim 300$ GeV.
Thus, we can safely neglect the Majorana mass terms in our
discussion.

Such a framework allows us to have highly suppressed Majorana mass
terms and results in the following R--symmetric gaugino--Higgsino
mass matrix:
\begin{equation}
\label{eq:mass_matrix}
{\mathcal{M}} \!\! =\!\!
\left[\begin{array}{c
c c c c c}
 0 & M_1 & 0 &  -\xi_1 m_Z s_W c_\beta & 0 & \xi_2 m_Z s_W s_\beta  \\
 M_1 & 0   & -m_Z s_W c_\beta & 0 &  m_Z s_W s_\beta & 0  \\
 0  & -m_Z s_W c_\beta & 0 & \mu_1 & 0 & 0  \\
 -\xi_1 m_Z s_W c_\beta & 0 & \mu_1 & 0 & 0 & 0 \\
  0  &  m_Z s_W s_\beta & 0 & 0 & 0 & \mu_2   \\
 \xi_2 m_Z s_W s_\beta & 0 & 0 & 0 & \mu_2 & 0\\
\end{array}\right]
\end{equation}
in the basis of $(\psi^0, \tilde{B}, \tilde{H}_d, \tilde{R}_u,
\tilde{H}_u, \tilde{R}_d)$. Note that, in order to make a
transparent discussion of the Dirac gaugino properties, we reduced
the number of free parameters by decoupling the wino component
which can be justified in the limit of heavy wino mass: $M_2\gg
M_1,|\mu_i|$.

The Dirac gaugino mass matrix (\ref{eq:mass_matrix}) can be
diagonalized by 6 angles which can be parameterized as
\begin{equation}
{\cal N} =
 \left[
{\begin{array}{cccccc}
c_1  & 0 & s_1 & 0 &  0 & 0 \cr
0 & c_4 & 0 & s_4 & 0  & 0 \cr
-s_1 & 0 & c_1 & 0 & 0 & 0 \cr
0 & -s_4 & 0 & c_4 & 0 & 0 \cr
0 & 0 & 0 & 0 & 1 & 0 \cr
0 & 0 & 0 & 0 & 0 & 1 \cr
\end{array}}
 \right]
 \left[
{\begin{array}{cccccc}
c_2  & 0 & 0 & 0 &  s_2 & 0 \cr
0 & c_3 & 0 & 0 & 0  & s_3 \cr
0 & 0 & 1 & 0 & 0 & 0 \cr
0 & 0 & 0 & 1 & 0 & 0 \cr
-s_2 & 0 & 0 & 0 & c_2 & 0 \cr
0 & -s_3 & 0 & 0 & 0 & c_3 \cr
\end{array}}
 \right]
 \left[
{\begin{array}{cccccc}
1 & 0 & 0 & 0 &  0 & 0 \cr
0 & 1 & 0 & 0 & 0  & 0 \cr
0 & 0 & c_5 & 0 & s_5 & 0 \cr
0 & 0 & 0 & c_6 & 0 & s_6 \cr
0 & 0 & -s_5 & 0 & c_5 & 0 \cr
0 & 0 & 0 & -s_6 & 0 & c_6 \cr
\end{array}}
\right]
.
\end{equation}
The six angles are defined by the diagonalization condition:
${\cal M}_{diag} = {\cal N}^T {\cal M} {\cal N}$,  where the
diagonalized mass matrix ${\cal M}_{diag}$ takes the diagonal form
of $2\times 2$ submatrices which have non-vanishing  symmetric
off-diagonal components of the Dirac mass eigenvalues denoted by
$m_\chi$, $m_{\psi_{H_1}}$, and $m_{\psi_{H_2}}$.

The sizes of the mixing angles play an important role in
determining the cosmic antiproton flux and the direct detection
rate as we will discuss in detail in later sections. It is now
instructive to find their approximate expression in the limit of
small mixing angles: $s_i \ll 1$.  In the leading order of  $m_Z
s_W \ll M_1 < \mu_{1,2}$,  the four mixing angles are given by
\begin{eqnarray} \label{si-approx}
&& s_1 \approx {c_1 m_Z s_W c_\beta (M_1 + \xi_1 \mu_1) \over M_1^2-\mu_1^2} \,,\quad
 s_2 \approx - {c_1 c_2 m_Z s_W s_\beta (c_4^2 M_1 + \xi_2 \mu_2) \over c_1^2 c_4^2 M_1^2- \mu_2^2}\;, \nonumber\\
&& s_3 \approx -{c_3 c_4 m_Z s_W s_\beta (c_1^2 \xi_2 M_1 +\mu_2) \over c_1^2 c_4^2 M_1^2-\mu_2^2} \,,\quad
 s_4  \approx  {c_4 m_Z s_W c_\beta (\xi_1 M_1 +\mu_1) \over M_1^2-
 \mu_1^2}\;,
\end{eqnarray}
and correspondingly the approximate mass eigenvalues are
\begin{eqnarray}
 && m_{\chi} \approx (c_1 c_2 M_1 + s_1 c_2 m_Z s_W c_\beta - s_2 m_Z s_W s_\beta) c_3 c_4 \nonumber\\
&& ~~~~~~  - (c_1 c_2 \xi_2 m_Z s_W s_\beta - s_2 \mu_2) s_3
         +(c_1 c_2 \xi_1 m_Z s_W c_\beta + s_1 c_2 \mu_1) c_3 s_4\;, \nonumber\\
 && m_{\psi_{H_1}} \approx
           (s_1 M_1-c_1 m_Z s_W c_\beta) s_4+(-s_1 \xi_1 m_Z s_W c_\beta+c_1 \mu_1) c_4\;, \nonumber\\
 && m_{\psi_{H_2}} \approx
       (s_3 c_4 M_1+c_3 \xi_2 m_Z s_W s_\beta) c_1 s_2
    +(s_3 c_4 m_Z s_W s_\beta+c_3 \mu_2) c_2\;.
\end{eqnarray}
Also in the limit of small $s_i$ and $\xi_i=1$, the remaining two
mixing angles have the form of
\begin{equation}
s_5 \approx s_6 \approx \frac{m_Z^2 s_W^2 s_\beta}{\mu_1 -
\mu_2}\; \left( \frac{c_\beta}{\mu_1} + \frac{1}{\mu_2} \right)
\;.
\end{equation}

After the diagonalization, one can find the following interaction
vertices of the dark matter particle $\chi$ relevant for our
analysis:
\begin{eqnarray}
\mathcal{L}_{f} &=&
 \sqrt{2}g'  Y_{f_R} {\cal N}_{22} [\overline{f}P_L\chi\widetilde{f}_R  +\overline{\chi}P_Rf\widetilde{f}^*_R] \nonumber\\
 &+& \sqrt{2}g' Y_{f_L} {\cal N}_{22} [\overline{f}P_R\chi^c\widetilde{f}_L
+\overline{\chi}^c P_Lf\widetilde{f}^*_L]\;, \\
\mathcal{L}_{h^0} &=& \frac{g'}{2}  h^0
[ C_1 (\overline{\psi}_{H_1}P_R\chi^c+\overline{\chi}^c P_L \psi_{H_1}) \nonumber\\
&& ~~~~~~~ +  C_2  (\overline{\psi}_{H_2} P_R \chi^c + \overline{\chi}^c P_L \psi_{H_2})
 \nonumber\\
&& ~~~~~~~ + C'_1 (\overline{\psi}_{H_1}P_L\chi^c+\overline{\chi}^c P_R \psi_{H_1}) \nonumber\\
&& ~~~~~~~ +  C'_2  (\overline{\psi}_{H_2} P_L \chi^c + \overline{\chi}^c P_R \psi_{H_2})
\nonumber\\
&& ~~~~~~~ + 2\delta_S \,\overline{\chi}\chi]\;, \label{chi-h} \\
\mathcal{L}_{Z} &=&
 \frac{g}{2c_W}\, Z_\mu
 [ \delta_1' ( \overline{\psi}_{H_1}\gamma_\mu P_L\chi^c
                +\overline{\chi}^c\gamma_\mu P_L \psi_{H_1}) \nonumber\\
&& ~~~~~~ +  \delta_1 ( \overline{\psi}_{H_1}\gamma_\mu P_R\chi^c
                 +\overline{\chi}^c\gamma_\mu P_R \psi_{H_1}) \nonumber\\
&& ~~~~~~ + \delta'_2 ( \overline{\psi}_{H_2}\gamma_\mu P_L\chi^c
                     +\overline{\chi}^c\gamma_\mu P_L \psi_{H_2}) \nonumber\\
&& ~~~~~~ + \delta_2 ( \overline{\psi}_{H_2}\gamma_\mu P_R\chi^c
                            +\overline{\chi}^c\gamma_\mu P_R
                            \psi_{H_2}) \nonumber\\
&& ~~~~~~ + \delta_V^2\, \overline{\chi}\gamma_\mu \chi
          + \delta_{A}^2\, \overline{\chi}\gamma_\mu\gamma_5
          \chi]\;,  \label{chi-Z}
\end{eqnarray}
where
\begin{eqnarray}  \label{couplings}
&& C_1 = s_\alpha{\cal N}_{22} {\cal N}_{33}
         + c_\alpha{\cal N}_{22} {\cal N}_{53} \;,\quad~~~~
C_2= c_\alpha{\cal N}_{22} {\cal N}_{55}
     + s_\alpha{\cal N}_{22} {\cal N}_{35} \;, \nonumber\\
&& C'_1 = \xi_1 s_\alpha{\cal N}_{11} {\cal N}_{44}
         + \xi_2 c_\alpha{\cal N}_{11} {\cal N}_{64}\;,\quad
C'_2= \xi_2 c_\alpha{\cal N}_{11} {\cal N}_{66}
    + \xi_1 s_\alpha{\cal N}_{11} {\cal N}_{46}\;, \nonumber\\
&& \delta_S={1\over2}\; (s_\alpha{\cal N}_{22} {\cal N}_{31} +
c_\alpha{\cal N}_{22} {\cal N}_{51} +\xi_1 s_\alpha{\cal N}_{11}
{\cal N}_{42}+ \xi_2 c_\alpha{\cal N}_{11} {\cal N}_{62} )\;,
\nonumber\\
&& \delta_1 = - {\cal N}_{44} {\cal N}_{42}
              + {\cal N}_{64} {\cal N}_{62}\;,\quad
   \delta_2 = + {\cal N}_{66} {\cal N}_{62}
              - {\cal N}_{46} {\cal N}_{42}\;,  \nonumber\\
&& \delta'_1 = - {\cal N}_{33} {\cal N}_{31}
               + {\cal N}_{53} {\cal N}_{51}\;, \quad
   \delta'_2 = + {\cal N}_{55} {\cal N}_{51}
               - {\cal N}_{35} {\cal N}_{31}\;,  \nonumber\\
&& \delta_V^2 = {1\over2}\; ({\cal N}_{31}^2 - {\cal N}_{51}^2 +
{\cal N}_{42}^2 - {\cal N}_{62}^2)\;,
\nonumber\\
&& \delta_{A}^2 = {1\over2\;} ({\cal N}_{31}^2 - {\cal N}_{51}^2 -
{\cal N}_{42}^2 + {\cal N}_{62}^2)\;.
\end{eqnarray}
Here $Y_{f_{L/R}}$ is the $U(1)$ hypercharge of the
left/right-handed fermion $f_{L/R}$ and the corresponding sfermion
$\tilde{f}_{L/R}$. The angle $\alpha$ is the usual diagonalization
angle of the neutral CP even Higgs bosons. In order to simplify
the discussion in our analysis, we will decouple all heavy Higgs
bosons by assuming $m_A\gg m_Z$, where $m_A$ is the pseudoscalar
Higgs boson mass.

\section{Indirect and direct signals of Dirac neutralino DM}

In the standard Majorana case, the direct annihilation of two
neutralinos to two fermions requires a helicity flip in the final
states and is vanishing in the limit of massless fermions,
$m_f=0$. As a consequence of this, the annihilation cross section
to light fermions is suppressed by a factor of $m^2_f/m^2_\chi$.
On the other hand, when the neutralino is a Dirac particle this
suppression is not present, so that the direct annihilation to
leptons is largely enhanced and can be the dominant annihilation
channel. In this case, the $t$--channel annihilation to quarks
through squark exchange can be suppressed if $m_{\tilde{q}} \gg
m_{\tilde{l}}$~\cite{park09}.

Then, in the presence of a large Higgsino component in the Dirac
neutralino composition, annihilations to gauge and Higgs bosons
can also lead to significant hadronic final states. Among them,
annihilations to quarks through a Higgs particle exchange are
suppressed either by a heavy pseudoscalar Higgs boson in the
decoupling limit, or by a suppressed s--wave contribution in the
non-relativistic limit, an effect which is present also in the
Majorana case.

Under these conditions, we analyze the dominant annihilation
channels and the direct detection bound of the Dirac neutralino
based on the results obtained in the previous section. In
Sections~\ref{subsec:ll_hz} and~\ref{subsec:z}, along with the
dominant annihilation of the Dirac neutralino to leptons we will
discuss the other relevant annihilation channels to hadronic final
states. We will present the neutralino--nucleon cross sections in
Section~\ref{subsec:direct}. The result of this section will be
used in Section~\ref{sec:dirac_neutralino} to constrain the
Higgsino component of the Dirac neutralino.

\subsection{Annihilations to $l\overline{l}$ and $h Z$}
\label{subsec:ll_hz}

First, let us consider the $t$--channel annihilation to leptons
through slepton exchange which has to be the dominant annihilation
channel to explain the observed energetic electron and positron
spectrum. In the case of  $m_{\widetilde{l}_R} \ll
m_{\widetilde{l}_L}$, we have
\begin{equation}
\langle\sigma v\rangle_{l\overline{l}} \simeq \mathcal{N}_{22}^4
\frac{2\pi\alpha^2}{c_W^4}\; Y_{l_R}^4\;
\frac{m_\chi^2}{(m_{\widetilde{l}_R}^2+m_\chi^2)^2}\;.
\label{eq:chichi_ll}
\end{equation}
On the other hand, the case of  $m_{\widetilde{l}_R} \simeq
m_{\widetilde{l}_L} \simeq m_{\widetilde{l}}$ leads to
\begin{equation}
\langle\sigma v\rangle_{l\overline{l}} \simeq \mathcal{N}_{22}^4
\frac{2\pi\alpha^2}{c_W^4}\; Y_l^4\;
\frac{m_\chi^2}{(m_{\widetilde{l}}^2+m_\chi^2)^2}\;,
\label{eq:chichi_ll_same}
\end{equation}
where $Y_l^4 \equiv Y_{l_R}^4+Y_{l_L}^4$. For the three families
of the sleptons having same masses, the above expression must be
multiplied by a factor of 3.

The Dirac gaugino $t$--channel annihilation through Higgsino
exchange produces a Higgs and a $Z$ bosons, which can
significantly contribute to the cosmic antiproton flux. The
annihilation rate for this mode is
\begin{eqnarray} \label{eq:sigmav_hz}
\langle\sigma v\rangle_{h Z} &\simeq&
\frac{\pi\alpha^2}{8c_W^4s_W^2} \;
\frac{\sqrt{m_\chi^2-\overline{m}_Z^2}}{m_\chi^3}  \\
&& \left\{
 \left(\frac{m_\chi^2}{m_Z^2}-1 \right) \left[ (y-z)^2 + (y'-z')^2
-\frac12 \frac{m_Z^2}{m_\chi^2} (z+z')^2 \right]  + \frac32
(y+y')^2  \right\}\;, \nonumber
\end{eqnarray}
where
$$
y = \sum_i \frac{m_\chi m_{\psi_{H_i}} C_i
\delta_i}{m_i^2},\;
y' = \sum_i \frac{m_\chi
m_{\psi_{H_i}} C'_i \delta'_i}{m_i^2},\;
z =
\sum_i \frac{m_\chi^2 C'_i \delta_i}{m_i^2},\;
z' =
\sum_i \frac{m_\chi^2 C_i \delta'_i}{m_i^2}\;,
$$
with $m_i^2 \equiv m_{\psi_{H_i}}^2 + m_\chi^2 -
\overline{m}_Z^2$, $\overline{m}_Z^2 \equiv (m_Z^2+m_h^2)/2$. Here
$m_h^2 - m_Z^2 \ll m_\chi^2$ is assumed.

In Section~\ref{sec:analysis}, we will present numerical results
on the limit of $\langle\sigma v\rangle_{h Z}$ coming from cosmic
antiproton fluxes. It is, however, useful to see a qualitative
behavior of the small mixing limit: $\delta_i, \delta'_i \ll 1$.
Taking $\xi_i=1$ in Eq.~(\ref{si-approx}),  the cross section
(\ref{eq:sigmav_hz}) reduces to a simple approximated form in the
zeroth order of $m_Z^2$:
\begin{equation}
\langle\sigma v\rangle_{h Z} \approx
\frac{\pi\alpha^2}{4c_W^4}\;
\frac{m_\chi^2}{(m_{\widetilde{H}}^2+m_\chi^2)^2}\; \left( 1
-\frac{m_\chi}{m_{\widetilde{H}}} \right)^2 \sin^2(\alpha+\beta)
\;,
\end{equation}
where $m_{\psi_{H_1}} \simeq m_{\psi_{H_2}} \simeq
m_{\widetilde{H}}$ and $M_1 \ll |\mu_i|$ is assumed. The ratio
between (\ref{eq:chichi_ll_same}) and (\ref{eq:sigmav_hz}) becomes
\begin{equation}
{ \langle\sigma v\rangle_{h Z} \over \langle\sigma
v\rangle_{l\overline{l}} } \approx {1 \over 8 Y_l^4}
\frac{(m_{\widetilde{l}}^2+m_\chi^2)^2}{(m_{\widetilde{H}}^2+m_\chi^2)^2}
\left( 1 - \frac{m_\chi}{m_{\widetilde{H}}} \right)^2
\sin^2(\alpha+\beta) \;.
\end{equation}
Assuming now $m_{\widetilde{l}} \simeq m_{\widetilde{H}}$ and
$Y_l^4 = 51/16$ (three even leptophilic), we have:
\begin{equation} \label{cross_ratio}
{ \langle\sigma v\rangle_{h Z} \over \langle\sigma
v\rangle_{l\overline{l}} } < \frac{2}{51} \left( 1 -
\frac{m_\chi}{m_{\widetilde{H}}} \right)^2 < \frac{2}{51} \;.
\end{equation}
Comparing the annihilation cross section to charged leptons
compatible with the PAMELA positron excess~\cite{PAMELA} and the
upper bound on the annihilation cross section to $hZ$ from the
PAMELA antiproton data~\cite{pbar}, presented in
Fig.~\ref{fig:leptophilic} of Section~\ref{sec:analysis}, we
obtain a conservative limit of  $\langle\sigma v\rangle_{h Z}/
\langle\sigma v\rangle_{l\overline{l}} \lsim 0.3$ which can be
easily satisfied, as shown in Eq. (\ref{cross_ratio}). In addition,
even for only one lepton channel, the condition is also satisfied:
$ \langle\sigma v\rangle_{h Z} / \langle\sigma
v\rangle_{l\overline{l}} < 2/17 < 0.3$.

\subsection{Annihilations through Z}
\label{subsec:z}

In the zero--velocity limit, the following annihilation channels
through $s$--channel exchange of a $Z$ boson have non-vanishing
amplitudes. Compared to Eq.~(\ref{eq:sigmav_hz}), these rates
contain an extra factor
 $\sim (m_\chi^2/m_{Z,W}^2)\, \delta^2$ and thus can be  important
in certain parameter regions.

The annihilation rate for $\chi\bar{\chi} \to f\overline{f}$ is
\begin{eqnarray}
\langle\sigma v\rangle_{f\overline{f}} &\simeq&
\frac{2\pi\alpha^2}{c_W^4s_W^4}\; \frac{\sqrt{m_\chi^2-m_f^2}}{m_\chi}\\
&& \left\{\frac{m_f^2}{m_Z^4}g_A^2\delta_A^4 +
\frac{m_\chi^2}{(4m_\chi^2-m_Z^2)^2}\left[2(g_V^2+g_A^2)
+\frac{m_f^2}{m_\chi^2}(g_V^2-2g_A^2) \right] \delta_V^4
\right\}\;, \nonumber
\end{eqnarray}
where $g_V=(T_3-2Q_f s_W^2)/2$ and $g_A=-T_3/2$.
The annihilation rates for $\chi\bar{\chi} \to h Z$ and $W^+ W^-$
are respectively given by
\begin{eqnarray}
\langle\sigma v\rangle_{hZ} &\simeq&
\frac{\pi\alpha^2}{c_W^4s_W^4}\;
\frac{\sqrt{m_\chi^2-\overline{m}_Z^2}}{m_\chi} \label{eq:sigmav_hz_z} \\
&&
\left[\frac{m_\chi^2}{m_Z^4}\left(1-\frac{m_Z^2}{m_\chi^2}\right)\delta_A^4
+\frac{m_\chi^2}{(4m_\chi^2-m_Z^2)^2}\left(1+\frac{2m_Z^2}{m_\chi^2}
\right) \delta_V^4 \right]\;, \nonumber \\
\langle\sigma v\rangle_{WW} &\simeq& \frac{\pi\alpha^2}{s_W^4}\;
\frac{m_\chi \sqrt{m_\chi^2-m_W^2}}{(4m_\chi^2-m_Z^2)^2}
\left(4\frac{m_\chi^4}{m_W^4}+16\frac{m_\chi^2}{m_W^2}-17-3\frac{m_W^2}{m_\chi^2}
\right) \delta_V^4\;. \label{eq:sigmav_ww}
\end{eqnarray}
Finally, there is also an annihilation channel $\chi\bar{\chi} \to
2h$. The annihilation rate for this channel is given by
\begin{eqnarray}
\langle\sigma v\rangle_{2h} \simeq
\frac{\pi\alpha^2}{4c_W^4s_W^4}\;
\frac{(m_\chi^2-m_h^2)^{3/2}}{m_\chi(4m_\chi^2-m_Z^2)^2}\;
\delta_V^4 \;.
\end{eqnarray}
Among these four channels, the process $\chi\bar{\chi} \to 2h$ is
the smallest one. The $hZ$ channel is larger than the
$f\overline{f}$ channel even for the top quark. Thus, the dominant
channels are $hZ$ or $W^+W^-$. The ratio between the two channels
is approximately $\delta_A^4 : \delta_V^4/4$. The ratio between
the cross sections for annihilations to $l\overline{l}$ and
$W^+W^-\; (hZ)$ depends on two parameters, $m_\chi$ and
$\delta_V\; (\delta_A)$. The upper bound on the ratio between the
annihilation rates for $\chi\bar{\chi} \to l\overline{l}$ and $W^+
W^-$ ($hZ$) is approximately 0.5 (0.3), as can be seen from
Fig.~\ref{fig:leptophilic}. Then, comparing (\ref{eq:sigmav_ww})
and (\ref{eq:sigmav_hz_z}) with (\ref{eq:chichi_ll_same}), one
finds the limits: $\delta_V \lesssim 0.3-0.03$ and $\delta_A
\lesssim 0.2-0.02$ depending on $m_\chi$ in the mass range 200 GeV
$\le m_\chi \le$ 2000 GeV. Note that the upper limit of $\delta_V$
is close to the current sensitivity of the direct detection of DM
as will be discussed in the following subsection (see
Fig.~\ref{DirectDetec}).  This will be also confirmed by our
numerical analysis performed in a more general parameter space.

\subsection{Direct detection through $Z$ and $h$ exchange}
\label{subsec:direct}

The vector interaction via $t$--channel $Z$ boson exchange
(\ref{chi-Z}) leads to a {\em spin--independent}
neutralino--nucleon cross section. The cross section for the
neutralino--nucleon vector interaction is given by
\begin{align}
\sigma^{\chi-n, p}_{\rm vector} \simeq \delta_V^4\; \frac{\pi
\alpha^2}{64 s_W^4 c_W^4}\; \frac{\mu_n^2}{m_Z^4}\;
\left[\frac{Z}{A} (1-2s_W^2)-\frac12 \right]^2\;,
\label{eq:neutralino_nucleon_z_exchange}
\end{align}
where $\mu_n$ is the reduced mass for $\chi$-nucleon, and $Z$ and
$A$ are the atomic number and the atomic weight of the target
nucleus, respectively.

\begin{figure}
\begin{center}
\includegraphics[width=0.82\linewidth]{fig_SI_detection}
\end{center}
\caption{Exclusion plot for the spin-independent neutralino--nucleon
cross section $\sigma_{\rm SI}$. The (blue) thick solid lines are
the cross sections via the vector interaction corresponding to
$\delta_V=0.3$, 0.2, 0.1, and 0.07, respectively. The (red) dashed
lines are the cross sections through the Higgs exchange corresponding
to $\delta_S=0.8$, 0.3, and $0.1$, respectively, taking $m_h=115$ GeV.
The dot--dashed line shows the CDMS II limit~\cite{CDMS}.}
\label{DirectDetec}
\end{figure}

In addition to the vector interaction, the Dirac gaugino $\chi$
interacts with nucleons through $t$--channel Higgs exchange
(\ref{chi-h}). The neutralino--nucleon cross section for the
scalar interaction is
\begin{align}
\sigma^{\chi-n, p}_{\rm scalar} \simeq \delta_S^2\; \frac{0.14^2
\times 4 g'^2 h_{hss}^2}{\pi}\; \frac{\mu_n^2 m_n^2}{m_h^4
m_s^2}\;,\label{eq:neutralino_nucleon_h_exchange}
\end{align}
where $h_{hss}$ is the Higgs--s quark--s quark Yukawa coupling. In
the decoupling limit, this result is estimated as
\begin{align}
\sigma^{\chi-n, p}_{\rm scalar} \simeq \delta_S^2\; \frac{0.14^2
\times 16 \pi \alpha^2}{s_W^2 c_W^2}\; \frac{\mu_n^2 m_n^2}{m_h^4
m_W^2}\;.
\end{align}

In Fig.~\ref{DirectDetec}, we present the neutralino--nucleon
cross sections via the vector interaction (thick solid lines) as a
function of $m_\chi$ for $\delta_V=0.3$, 0.2, 0.1, and 0.07. The
scalar interaction cross sections (dashed lines) are also shown as
a function of $m_\chi$ for $\delta_S=0.8$, 0.3, and 0.1. The limit
from the CDMS II experiment~\cite{CDMS} is shown as a dot--dashed
line.

\section{Analysis}\label{sec:analysis}

In this section, we analyze the phenomenology of Dirac gauginos in
a quantitative way. As discussed in the previous sections, Dirac
gauginos can easily meet the requirements of a leptophilic DM
candidate, and so we will start in Section~\ref{sec:leptophilic}
by summarizing present constraints on generic leptophilic models.
We will then proceed in Section~\ref{sec:bino_leptophilic} to
discuss specific properties of Dirac binos as leptophilic DM,
while in Section~\ref{sec:dirac_neutralino} we will extend the
analysis to Dirac neutralinos of generic composition in some
particular examples.

\subsection{Constraints on leptophilic dark matter}
\label{sec:leptophilic}

Leptophilic DM annihilation is usually advocated in order to
explain simultaneously the PAMELA positron excess~\cite{PAMELA}
and the excellent agreement between the observed antiproton
spectrum and the corresponding standard expectation \cite{pbar}.
The present situation of a leptophilic DM candidate annihilating
democratically into charged leptons of the three families is
summarized in Fig.~\ref{fig:leptophilic}, where the annihilation
cross section $\langle\sigma v\rangle$ is plotted as a function of
the DM mass $m_{\chi}$.
\begin{figure}
\begin{center}
\includegraphics[bb=51 230 505 645,width=0.80\linewidth]{dirac_gaugino_leptophilic.ps}
\end{center}
\caption{Annihilation cross section times velocity $\langle\sigma
  v\rangle$ for a DM candidate annihilating democratically to charged
  leptons of the three families as a function of the mass
  $m_{\chi}$. The thick solid contour shows the range of values
  compatible with the PAMELA positron excess~\cite{PAMELA}; the thin
  solid contour is the range compatible to the observed $e^{+}+e^{-}$
  flux measured by FERMI--LAT~\cite{FERMI}; the thin dot--dashed line
  is the 2 $\sigma$ upper bound from the observed $e^{+}+e^{-}$ flux
  of FERMI; the thick dot--dashed line is the 2 $\sigma$ upper bound
  from the $e^{+}+e^{-}$ HESS measurement~\cite{HESS}; the short
  dash--long dash line represents the upper bound on $\langle\sigma
  v\rangle$ from CMB~\cite{cmb_galli,cmb_slatyer,cmb_padmanabhan}. The
  lower and upper dotted lines show the upper bound on $\langle\sigma
  v\rangle$ obtained by comparing the expected gamma--ray flux
  produced by Inverse Compton (IC) scattering of the final state
  leptons to the FERMI--LAT measurement of the diffuse gamma ray
  emission with or without subtraction of the expected standard
  background, respectively~\cite{FERMI_diffuse}. The short dashed and
  long dashed lines respectively show the upper bounds on the annihilation cross
  section to the final states $W^+W^-$ and $hZ$ from the PAMELA antiproton
  data~\cite{pbar}. See Section \protect\ref{sec:analysis} for
  details.}\label{fig:leptophilic}
\end{figure}
In particular, the thick and thin closed solid contours show the
range of values compatible with the PAMELA positron
excess~\cite{PAMELA} and the FERMI--LAT $e^{+}+e^{-}$
data~\cite{FERMI}, respectively. The contours are calculated by
requiring that the $\chi^2$ per degree of freedom for fits to the
data is less than or equal to 1 (only PAMELA data above 10 GeV
have been included in the fit), and assuming for the secondary
positron and electron backgrounds the conventional GALPROP model
denominated by Model \#0 in Table 1 of \cite{fermi09}. As far as
the propagation model for primary electrons and positrons is
concerned, we have adopted a Navarro--Frenk--White (NFW)
profile~\cite{NFW} with medium ranges for the diffusion
coefficient and for the size of the propagation region,
corresponding to the model NFW--med in Table 2 of \cite{cirelli}.
The two dot--dashed lines in the upper part of
Fig.~\ref{fig:leptophilic} represent conservative 2 $\sigma$ C.L.
upper bounds for $\langle\sigma v\rangle$ obtained from the flux
of $e^{+}+e^{-}$ observed by FERMI \cite{fermi09} (thin line) and
the $e^{+}+e^{-}$ flux measured by HESS \cite{HESS} (thick line).

In the same Figure, we also plot for reference with the short
dash--long dash line the upper bound on $\langle\sigma v\rangle$
obtained by considering the imprint on the Cosmic Microwave Background
Radiation (CMB) from the injection of charged leptons from DM
annihilations at the recombination
epoch~\cite{cmb_galli,cmb_slatyer,cmb_padmanabhan}. In particular, the
plotted line is obtained by taking the WMAP5 constraint on the
quantity $f \langle\sigma v\rangle$ from Figure 4 of
Ref.~\cite{cmb_galli}, where $f$ is defined as the average fraction of
the DM rest energy deposited in the gas at $z\simeq$ 800--1000, and
taking $f\simeq 0.39$ from the analysis of Ref.~\cite{cmb_slatyer}. As
one can see, at present the effect of the CMB constraint on
leptophilic models which can explain the PAMELA excess is limited to
very large masses, $m_{\chi}\gsim$ 1.5 TeV. Future polarization data
from Plank will be able to improve this kind of limits
considerably~\cite{cmb_padmanabhan}.

Finally\footnote{Signals from DM annihilation in the Galactic
Center are very sensitive to the choice of density profile.
Therefore, we do not consider them here.}, the dotted lines show
the upper bounds on $\langle\sigma v\rangle$ obtained by comparing
the expected gamma--ray flux produced by Inverse Compton (IC)
scattering of the final state leptons to the diffuse flux of
gamma--rays measured by FERMI at intermediate Galactic
latitudes~\cite{FERMI_diffuse}. We do not include in our analysis
the preliminary data points very recently released by the
FERMI--LAT Collaboration. Due to the large experimental errors,
they would not change our conclusions~\cite{FERMI_preliminary}.
The upper dotted line has been obtained by directly comparing the
flux expected from leptophilic DM (calculated in the approximation
of Ref.~\cite{cirelli_ic}) to the FERMI--LAT data, while the lower
dotted curve has been obtained by subtracting the estimation of
the standard background from the data (as a conservative
estimation of the latter we have assumed the lower boundary of the
dashed region indicated as ``Total'' in the left--hand panel of
Fig.~1 of Ref.~\cite{FERMI_diffuse}).

The IC analysis is described in detail in
Fig.~\ref{fig:inverse_compton}, where the diffuse FERMI--LAT data
at latitudes $10^\circ < b < 20^\circ$ from \cite{FERMI_diffuse}
as a function of the gamma--ray energy $E_{\gamma}$ are compared
with the corresponding fluxes from leptophilic DM annihilations.
\begin{figure}
\begin{center}
\includegraphics[bb=23 200 505 645,width=0.80\linewidth]{dirac_gaugino_inverse_compton.ps}
\end{center}
\caption{ Diffuse gamma--ray flux produced by Inverse Compton
  scattering of the final state electrons produced in DM annihilations as
  a function of the gamma--ray energy $E_{\gamma}$ for a leptophilic
  DM candidate annihilating democratically to charged leptons of the
  three families.  The lower solid curves represent the gamma--ray
  fluxes from DM annihilation for the representative values
  $m_{\chi}$=200, 500, 1000, 1500, and 2000 GeV from bottom to top,
  where for each $m_{\chi}$ the value of $\langle\sigma v\rangle$
  is taken from the lower boundary of the thick solid contour of
  Fig.~\protect\ref{fig:leptophilic} (adopted as a conservative estimation
  for the annihilation cross section required to explain the PAMELA
  data). The same expected fluxes are also summed to the standard
  background, shown by the thick solid line in the range 0.1 GeV $\le
  E_{\gamma} \le$ 10 GeV, and the results are plotted in the same
  energy range. The dashed curves correspond to the IC predictions for
  the additional value $m_{ \chi}\simeq$ 1135 which, as shown in the
  magnified inset at the upper--right, can be adopted as an estimation
  of the upper bound for $m_{\chi}$ from the IC flux from our
  analysis.  The experimental points are the FERMI--LAT data at
  latitudes $10^\circ < b < 20^\circ$ from \cite{FERMI_diffuse}.
}\label{fig:inverse_compton}
\end{figure}
In particular, the lower solid curves represent the gamma--ray
fluxes from DM annihilation for the representative values
$m_{\chi}$=200, 500, 1000, 1500, and 2000 GeV (from bottom to
top), where for each $m_{\chi}$ the value of $\langle\sigma
v\rangle$ is taken from the lower boundary of the thick solid
contour of Fig.~\ref{fig:leptophilic} (that we adopt here and in
the following as a conservative estimation for the annihilation
cross section required to explain the PAMELA data). The same
expected fluxes are also summed to the standard background, shown
by the thick solid line in the range 0.1 GeV $\le E_{\gamma} \le$
10 GeV, and the results are plotted in the same energy range. The
dashed curves correspond to the predictions for the additional
value $m_{ \chi}\simeq$ 1135 which, as shown in the magnified
inset at the upper--right, can be adopted as an estimation of the
upper bound for $m_{\chi}$ from the IC flux.

A comment is in order here. Following other similar analysis in
the literature \cite{fermi09,cirelli}, we take the results shown
in Fig.~\ref{fig:leptophilic} as only indicative of the present
trends. In fact, it is clear that a consistent $\chi^2$ analysis
would require a robust assessment of the systematic uncertainties,
an established knowledge of the expected backgrounds\footnote{At
  variance with antiprotons, the expected standard background for
  electrons and positrons could in principle be only in part of
  secondary origin, with a sizable primary fraction (see for
  instance \cite{profumo,blasi}).} and a full marginalization over
the astrophysical parameters, something which is not possible in
light of the present uncertainties.

\subsection{The Dirac bino as a leptophilic DM candidate}
\label{sec:bino_leptophilic}

Dirac gauginos can easily meet the requirements of a leptophilic
DM candidate, since their annihilation cross section to leptons
can be dominant, not being chirality flip suppressed as in the
case of Majorana gauginos, while annihilations to quarks
potentially capable of producing an excess in the antiproton
signal can be inhibited by assuming large masses for the squarks
\cite{park09}. If the additional hadronic annihilation channels
discussed in Sections~\ref{subsec:ll_hz} and~\ref{subsec:z} are
further suppressed by assuming a negligible Higgsino component in
the neutralino composition (by taking $|\mu_{1,2}| \gg M_1$ in the
mass matrix of Eq.~(\ref{eq:mass_matrix})), a totally leptophilic
model is obtained for which only the constraint $m_{\chi}\lsim$ 1
TeV from the IC flux discussed in Fig.~\ref{fig:inverse_compton}
is applied\footnote{Notice
  that the IC gamma--ray flux retains the directional information of
  the source, allowing in principle to establish whether the e$^{\pm}$
  PAMELA excess is diffused in all the Galactic halo or localized, for
  instance, in a DM clump close to the Solar System. The preliminary
  data of Ref.~\cite{FERMI_diffuse} do not provide this piece of
  information since they are averaged over all galactic longitudes
  $0^\circ \le l \le 180^\circ$.}. The phenomenology of such a DM
candidate is quite simple, and is summarized in
Fig.~\ref{fig:boost_factor}, where the solid lines show the ratio
between the annihilation cross section $\langle\sigma v\rangle$
required to explain the PAMELA data (taken as before from the lower
boundary of the thick closed solid contour in
Fig.~\ref{fig:leptophilic}) and that calculated by making use of
Eq.~(\ref{eq:chichi_ll_same}) for $m_{\widetilde{l}}/m_{\chi}=$1 (thin
line) and 2 (thick one).
\begin{figure}
\begin{center}
\includegraphics[bb=51 230 505 645,width=0.70\linewidth]{dirac_gaugino_boost_factors.ps}
\end{center}
\caption{Boost factors for a Dirac gaugino DM candidate annihilating
  democratically to leptons of the three families as a function of the
  mass and in the limit $|\mu|\gg M_1$. Solid lines show the ratio
  between the annihilation cross section required to explain the
  PAMELA excess and the value of $\langle\sigma v\rangle$ calculated using
  Eq.~(\protect\ref{eq:chichi_ll_same}). Dashed lines show the ratio
  between the observed lower value of the DM relic density
  $\Omega_{min} h^2=0.098$ \protect\cite{WMAP} and the corresponding
  thermal relic abundance for the Dirac gaugino. Thin lines
  refer to $m_{\widetilde{l}}/m_{\chi}=$ 1 (where we have assumed a small
  mass splitting between $m_{\widetilde{l}}$ and $m_{\chi}$ sufficient to
  avoid coannihilations between sleptons and neutralinos) while thick
  ones to $m_{\widetilde{l}}/m_{\chi}=$2, where $m_{\widetilde{l}}$ is the slepton
  mass.}\label{fig:boost_factor}
\end{figure}
In particular, $m_{\widetilde{l}}/m_{\chi}\gsim $1 maximizes the
expected annihilation cross section by assuming the lightest
possible slepton mass compatible with the requirement that the
neutralino is the Lightest Supersymmetric Particle (LSP). In this
latter case, the Dirac gaugino annihilation cross section to
leptons can explain the PAMELA data for $m_{\chi}\simeq$ 330 GeV,
while $m_{\chi}\simeq$ 200 GeV is needed if
$m_{\widetilde{l}}/m_{\chi}=$2.

It is well known, however, that the values of the annihilation
cross section that can explain the PAMELA excess ($\langle\sigma
v\rangle \simeq 10^{-24}$ cm$^3$ s$^{-1}$) are about two orders of
magnitude larger than the range compatible to a standard thermal
relic abundance in agreement with observation (2--3$ \times
10^{-26}$ cm$^3$ s$^{-1}$ at the decoupling temperature $T\simeq
m_{\chi}/20$). This is naively shown in
Fig.~\ref{fig:boost_factor}, where the dashed lines represent the
ratio between the 2 $\sigma$ lower value of the observed DM relic
density $\Omega_{min} h^2=0.098$~\cite{WMAP} and the corresponding
thermal relic abundance for the Dirac gaugino. The thin dashed
line refers to $m_{\widetilde{l}}/m_{\chi}=$ 1 while the thick one
to $m_{\widetilde{l}}/m_{\chi}=$ 2. From this figure, one can see
that a light Dirac gaugino ($m_{\chi}\lsim$ 500 GeV) can explain
the PAMELA data with moderate or no boost factor at all if, for
instance, some non-standard expansion history of the Universe
\cite{quintessence} or non-thermal production mechanism is
advocated in order to reconcile its DM relic abundance to the
observation. Alternatively, a thermal relic density in agreement
with observation is attained for $m_{\chi}\gsim$ 800 GeV, but in
this case a large enhancement of the annihilation cross section to
leptons is necessary. Such an enhancement could be provided by an
astrophysical boost factor due to substructures, although recent
analysis seems to disfavor values larger than order 10
\cite{clumpiness}. Furthermore, this piece of information can be
combined to the data on $e^++e^-$ from FERMI--LAT, which, as shown
by the thin closed contour plot in Fig.~\ref{fig:leptophilic},
imply a lower bound on the neutralino mass $m_{\chi} \gsim$ 465
GeV.  Notice, however, that lower values for the mass of the
annihilating DM particle can be in principle assumed if some
additional contribution to the electron+positron background is
claimed at energies $E\gsim 1$ TeV to explain the FERMI--LAT data
independently~\cite{profumo,blasi,extragalactic_source}.

\subsection{The case of a Dirac neutralino of general composition}
\label{sec:dirac_neutralino}

As discussed in Section~\ref{subsec:direct}, an important
phenomenological feature of a Dirac neutralino is the presence of
a vector coupling with the $Z$ boson, which on the other hand is
vanishing in the Majorana case. This implies that, while in the
standard Majorana scenario a diagram with the $Z$ boson exchange
can only contribute to the spin--dependent neutralino--nucleon
cross section,\footnote{The most stringent limits on pure
  WIMP--proton and WIMP--neutron spin--dependent cross sections
  are given by KIMS~\cite{KIMS} and ZEPLIN-III~\cite{ZEPLIN-III_SD},
  respectively.} for the Dirac case it can lead to a much more
sizeable cross section enhanced by a factor of $\simeq A^2$
(see Eq.~(\ref{eq:neutralino_nucleon_z_exchange})). However, note
that the coupling between a neutralino and a $Z$ boson vanishes
(as long as the coupling to the Higgs bosons) in the limit
$|\mu_{1,2}|\gg M_1$ of a pure gaugino. This implies that the
detection of Dirac neutralinos through direct searches is possible
only in the presence of a Higgsino component in a Dirac neutralino
of arbitrary composition.  In order to explore this possibility,
we discuss in this section the full parameter space of our model,
by allowing $|\mu_{1,2}|\simeq M_1$, and discuss the constraints
coming from the hadronic annihilation channels discussed in
Sections \ref{subsec:ll_hz} and \ref{subsec:z}. In particular, in
Figs. \ref{fig:m1_mu_ratio_1} and \ref{fig:m1_mu_ratio_0.1}, the
$M_1-\mu_{i}$ parameter space of the Dirac neutralino is explored
for the two representative cases $\mu_1/\mu_2=1$ and
$\mu_1/\mu_2=0.1$. Our numerical analysis is performed in the case
of $\xi_1=\xi_2=1$.
\begin{figure}
\begin{center}
\includegraphics[bb=51 220 505 645,width=0.80\linewidth]{dirac_gaugino_m1_mu_1.ps}
\end{center}
\caption{Parameter space for a Dirac neutralino of general
  composition, for $\mu_1$=$\mu_2$ and $\tan\beta$=3,10 (left and
  right panels, respectively). In each panel, the region below the
  slanted solid line is excluded by the PAMELA antiproton data, while
  along the two dotted lines the ratio between the neutralino--nucleon
  scattering cross section calculated with
  Eqs. [(\protect\ref{eq:neutralino_nucleon_z_exchange}),
    (\protect\ref{eq:neutralino_nucleon_h_exchange})] and the
  experimental limit from CDMS II~\cite{CDMS} is fixed to 1 (lower
  curve) and 10$^{-3}$ (upper curve). The regions below the lower
  dotted curves, where this ratio is larger than 1, are excluded by
  the direct detection constraint. Moreover, in each plane, the
  vertical thin dashed line to the left represents points where the
  boost factor, defined as the ratio between the annihilation cross
  section $\langle\sigma v\rangle$ required to explain the
  PAMELA excess and that
  calculated by making use of Eq.~(\protect\ref{eq:chichi_ll_same}),
  is equal to 10, while the vertical thick dot--dashed line to the right
  represents points at constant mass $m_{\chi}$=1 TeV.}
\label{fig:m1_mu_ratio_1}
\end{figure}
\begin{figure}
\begin{center}
\includegraphics[bb=51 220 505 645,width=0.80\linewidth]{dirac_gaugino_m1_mu_2.ps}
\end{center}
\caption{The same as in Fig.~\protect\ref{fig:m1_mu_ratio_1}, with
  $\mu_2/\mu_1$=10. In both panels, the three dotted lines show points
  where the ratio between the neutralino--nucleon scattering cross
  section calculated with
  Eqs. [(\protect\ref{eq:neutralino_nucleon_z_exchange}),
    (\protect\ref{eq:neutralino_nucleon_h_exchange})] and the
  experimental limit from CDMS II~\cite{CDMS} is fixed to 1 (lower
  curve, barely visible in the right--hand panel), 10$^{-3}$ (middle
  curve), and 10$^{-5}$ (upper curve).  }\label{fig:m1_mu_ratio_0.1}
\end{figure}
In each figure, the left--hand panel corresponds to $\tan\beta=3$
and the right--hand panel to $\tan\beta=10$. In all the
$M_1$--$\mu_i$ planes, the predominantly Higgsino region below the
slanted solid line is excluded by an antiproton flux above the
PAMELA data of Ref.~\cite{pbar}, driven by the cross section to
$W^+W^-$ of Eq.~(\ref{eq:sigmav_ww}) and a subdominant
contribution from the hZ final state of Eq.~(\ref{eq:sigmav_hz})
(in the calculation of the latter cross section we have assumed a
supersymmetric Higgs sector in the decoupling limit, $m_{H,A}\gg
m_h$, with $m_h$=115 GeV). The corresponding upper bounds to these
two cross sections, which as already mentioned in Sections
\ref{subsec:ll_hz} and \ref{subsec:z} turn out to be the dominant
hadronic ones in our R--symmetric scenario, are plotted for
reference in Fig.~\ref{fig:leptophilic} as short--dashed and
long--dashed lines, respectively. They have been obtained by
conservatively requiring $\chi^2<40$ when comparing the
theoretical expectation to the PAMELA data (this value corresponds
approximately to a 99.5 \% C.L. for 17 degrees of freedom). For
the calculation of the antiproton fluxes, we have adopted the
NFW--med model for propagation \cite{cirelli} and the
parametrization of Ref.~\cite{pbar_background} for the secondary
antiproton background.

In Figs.~\ref{fig:m1_mu_ratio_1} and \ref{fig:m1_mu_ratio_0.1},
the vertical thin dashed line to the left represents points where
the boost factor, defined as the ratio between the annihilation
cross section $\langle\sigma v\rangle$ required to explain the
PAMELA excess and that calculated by making use of
Eq.~(\protect\ref{eq:chichi_ll_same}), is equal to 10. In
particular, the points to the right of this vertical line require
a larger value. Note that an astrophysical enhancement to the
effective cross section provided by DM substructure larger than
order 10 appears to be unlikely \cite{clumpiness}. Moreover, in
each $M_1$--$\mu_i$ plane, the vertical thick dot--dashed line to
the right represents points with a constant Dirac neutralino mass
$m_{\chi}$=1 TeV. Configurations to the right of this line have
larger masses and appear to be disfavored by the IC flux shown in
Fig.~\ref{fig:inverse_compton}. Note that this is the only
irreducible astrophysical bound which is constraining also in the
pure gaugino limit $|\mu_i|\gg M_1$.

In the regions of Figs.~\ref{fig:m1_mu_ratio_1}
and~\ref{fig:m1_mu_ratio_0.1} that are excluded by antiproton
fluxes (below the slanted solid lines), a sizeable Higgsino
fraction can also drive the neutralino--nucleon cross section
above the present experimental limit. This is shown by the dotted
lines which represent configurations with a fixed ratio between
the expected neutralino--nucleus cross section and the present
experimental upper bound from CDMS II~\cite{CDMS}. In particular,
in all the $\mu_i-M_1$ planes this ratio is equal to 1, 10$^{-3}$,
and 10$^{-5}$ (if present), starting from the lower curve. In the
regions below the lower dotted curves, this ratio is larger than
one, so that they are excluded by the present limit from CDMS II.

The expected fluxes for positrons, electrons, and antiprotons, as
well as the expected direct detection cross section for a Dirac
neutralino are shown in detail in Fig.~\ref{fig:fluxes} for the
specific example $m_{\chi}\simeq 465$ and $\langle\sigma
v\rangle\simeq 1.4 \times 10^{-24}$ cm$^{-3}$ s$^{-1}$. This
configuration corresponds to the lower mass bound implied by the
FERMI-LAT $e^++e^-$ data if no additional sources of electrons and
positrons are assumed and, as shown in
Fig.~\ref{fig:boost_factor}, implies a boost factor of around 3 in
the case of $m_{\widetilde{l}}/m_{\chi}\simeq$1 and in the limit
of a pure bino. In particular, in Figs. \ref{fig:fluxes}a and
\ref{fig:fluxes}b, the corresponding positron and $e^++e^-$ fluxes
are plotted as a function of the energy, while the antiproton flux
and the neutralino--nucleon cross section are plotted in Figs.
\ref{fig:fluxes}c and \ref{fig:fluxes}d, respectively, for the
case of a Dirac neutralino of general gaugino--Higgsino
composition in the representative case of $\tan\beta=3$ and
$\mu_1/\mu_2$=1.
\begin{figure}
\begin{center}
\includegraphics[bb=51 220 505 645,width=0.4\linewidth]{pamela_positrons_mchi_465.ps}
\includegraphics[bb=51 220 505 645,width=0.4\linewidth]{fermi_electrons_mchi_465.ps}

\includegraphics[bb=51 220 505 680,width=0.4\linewidth]{pamela_antiprotons_mchi_465.ps}
\includegraphics[bb=51 220 505 680,width=0.4\linewidth]{sigma_mu.ps}
\end{center}
\caption{Various observables calculated for the representative
  configuration $m_{\chi}=465$ GeV and $\langle\sigma
  v\rangle_{l\overline{l}}=1.4\times 10^{-24}$ cm$^3$ s$^{-1}$. (a)
  Solid line: positron fraction compared to the PAMELA
  data~\cite{PAMELA}. Dashes: secondary background (Model \#0 of
  Ref.~\cite{fermi09}); (b) Solid line: electron+positron flux
  compared to the FERMI--LAT data~\cite{fermi09}. Dashes: secondary
  background (Model \#0 of Ref.~\cite{fermi09}); (c) Solid line:
  antiproton fraction compared to the PAMELA data~\cite{pbar}. Dashes:
  secondary background~\cite{pbar_background}. The value of the
  hadronic annihilation cross section $\langle\sigma
  v\rangle_{W^+W^-}$ used for the calculation corresponds to the
  configuration indicated with a star in panel (d) which is at the
  level of the experimental CDMS II exclusion plot; (d)
  Neutralino--nucleon cross section as a function of $\mu_1=\mu_2$ for
  $\tan\beta=3$. The horizontal line is the corresponding CDMS II
  upper bound~\cite{CDMS}.}\label{fig:fluxes}
\end{figure}
Note that in the case of a non-negligible Higgsino--gaugino mixing
the boost factor for the leptonic annihilation cross section
required to explain the PAMELA data, which is plotted in
Fig.~\ref{fig:boost_factor} in the pure gaugino limit $|\mu_i|\gg
M_1$, can be somewhat larger due to the suppression of the bino
coefficient $\mathcal{N}_{22}$. However, this effect is not
sizeable. For instance, for the maximal Higgsino composition
compatible to the CDMS II limit shown by a star in
Fig.~\ref{fig:fluxes}d the boost factor turns out to be $\simeq$4
instead of $\simeq$3.

\section{Conclusions}

Determining the Majorana/Dirac nature of gauginos will be an
interesting task for future experiments to look for supersymmetry.
Moreover, as an interesting variance of the standard Majorana
case, Dirac gauginos can be natural realizations of leptophilic
DM, which has been recently proposed to explain the rising
positron flux observed in cosmic rays by PAMELA without producing
excesses in the antiproton signal. In this paper, we have analyzed
the phenomenology of Dirac gauginos in a specific supersymmetric
realization, where a continuous R symmetry is assumed to protect
vanishingly small Majorana masses. We have shown that a light
Dirac gaugino ($m_{\chi}\lsim$ 500 GeV) can explain the PAMELA
data with moderate or no boost factor for light ($\gsim m_{\chi}$)
slepton masses. Furthermore, in the case of a non-vanishing
Higgsino fraction, Dirac gauginos can have a vector coupling with
the $Z$ gauge boson leading to a sizable spin--independent
scattering off nuclei. In some specific examples, we have shown
that present constraints on the Higgsino fraction of Dirac
gauginos from direct detection experiments are at the same level
of those coming from antiproton data. This implies that a Dirac
gaugino signal is potentially at the level of the sensitivity of
direct detection experiments at present and in the near future.

\medskip

{\bf Acknowlegement:} E.J.C. was supported by Korea Neutrino Research
Center through National Research Foundation of Korea Grant
(2009-0083526). S.S. was supported by the WCU program
(R32-2008-000-10155-0) of National Research Foundation of Korea.

redpajama_set_name: RedPajamaArXiv


text:
package com.zxq.adapter;

import android.content.ContentResolver;
import android.content.Context;
import android.content.Intent;
import android.database.Cursor;
import android.graphics.drawable.Drawable;
import android.text.Html;
import android.text.TextUtils;
import android.view.LayoutInflater;
import android.view.View;
import android.view.ViewGroup;
import android.widget.BaseExpandableListAdapter;
import android.widget.ImageView;
import android.widget.TextView;

import com.zxq.activity.FriendInfoActivity;
import com.zxq.db.RosterProvider;
import com.zxq.db.RosterProvider.RosterConstants;
import com.zxq.service.XmppService;
import com.zxq.util.*;
import com.zxq.xmpp.R;

import java.util.ArrayList;
import java.util.HashMap;
import java.util.List;

import org.jivesoftware.smackx.vcardtemp.packet.VCard;

public class RosterAdapter extends BaseExpandableListAdapter {
    // 不在线状态
    private static final String OFFLINE_EXCLUSION = RosterConstants.STATUS_MODE + " != " + StatusMode.offline.ordinal();
    // 在线人数
    private static final String COUNT_AVAILABLE_MEMBERS = "SELECT COUNT() FROM " + RosterProvider.TABLE_ROSTER + " inner_query" + " WHERE inner_query." + RosterConstants.GROUP + " = " + RosterProvider.QUERY_ALIAS + "." + RosterConstants.GROUP + " AND inner_query." + OFFLINE_EXCLUSION;
    // 总人数
    private static final String COUNT_MEMBERS = "SELECT COUNT() FROM " + RosterProvider.TABLE_ROSTER + " inner_query" + " WHERE inner_query." + RosterConstants.GROUP + " = " + RosterProvider.QUERY_ALIAS + "." + RosterConstants.GROUP;
    private static final String[] GROUPS_QUERY_COUNTED = new String[]{RosterConstants._ID, RosterConstants.GROUP, "(" + COUNT_AVAILABLE_MEMBERS + ") || '/' || (" + COUNT_MEMBERS + ") AS members"};
    // 联系人查询序列
    private static final String[] ROSTER_QUERY = new String[]{RosterConstants._ID, RosterConstants.JID, RosterConstants.ALIAS, RosterConstants.STATUS_MODE, RosterConstants.STATUS_MESSAGE,};
    private Context mContext;
    private ContentResolver mContentResolver;
    private List<Group> mGroupList;
    private boolean mIsShowOffline;// 是否显示离线联系人
    private LayoutInflater mInflater;
    private XmppService mXmppService;
    private HashMap<Integer, Integer> groupStatusMap;

    public RosterAdapter(Context context,XmppService mXmppService) {
        this.mContext = context;
        this.mXmppService = mXmppService;
        this.mInflater = LayoutInflater.from(context);
        this.mContentResolver = context.getContentResolver();
        this.mGroupList = new ArrayList<Group>();
        this.groupStatusMap = new HashMap<Integer, Integer>();
        this.mIsShowOffline = PreferenceUtils.getPrefBoolean(mContext, PreferenceConstants.SHOW_OFFLINE, true);
    }

    public void requery() {
        if (mGroupList != null && mGroupList.size() > 0)
            mGroupList.clear();
        // 是否显示在线人数
        mIsShowOffline = PreferenceUtils.getPrefBoolean(mContext, PreferenceConstants.SHOW_OFFLINE, true);
        String selectWhere = null;
        if (!mIsShowOffline)
            selectWhere = OFFLINE_EXCLUSION;
        Cursor groupCursor = mContentResolver.query(RosterProvider.GROUPS_URI, GROUPS_QUERY_COUNTED, selectWhere, null, RosterConstants.GROUP);
        groupCursor.moveToFirst();
        while (!groupCursor.isAfterLast()) {
            Group group = new Group();
            group.setGroupName(groupCursor.getString(groupCursor.getColumnIndex(RosterConstants.GROUP)));
            group.setMembers(groupCursor.getString(groupCursor.getColumnIndex("members")));
            mGroupList.add(group);
            groupCursor.moveToNext();
        }
        groupCursor.close();
        LogUtil.i("cursor size = " + mGroupList.size());
        notifyDataSetChanged();
    }

    protected List<Roster> getChildrenRosters(String groupname) {
        // Given the group, we return a cursor for all the children within
        // that group
        List<Roster> childList = new ArrayList<Roster>();

        String selectWhere = RosterConstants.GROUP + " = ?";
        if (!mIsShowOffline)
            selectWhere += " AND " + OFFLINE_EXCLUSION;
        Cursor childCursor = mContentResolver.query(RosterProvider.CONTENT_URI, ROSTER_QUERY, selectWhere, new String[]{groupname}, null);
        childCursor.moveToFirst();
        while (!childCursor.isAfterLast()) {
            Roster roster = new Roster();
            roster.setJid(childCursor.getString(childCursor.getColumnIndexOrThrow(RosterConstants.JID)));
            roster.setAlias(childCursor.getString(childCursor.getColumnIndexOrThrow(RosterConstants.ALIAS)));
            roster.setStatus_message(childCursor.getString(childCursor.getColumnIndexOrThrow(RosterConstants.STATUS_MESSAGE)));
            roster.setStatusMode(childCursor.getString(childCursor.getColumnIndexOrThrow(RosterConstants.STATUS_MODE)));
            childList.add(roster);
            childCursor.moveToNext();
        }
        childCursor.close();
        return childList;
    }

    @Override
    public int getGroupCount() {
        return mGroupList.size();
    }

    @Override
    public int getChildrenCount(int groupPosition) {
        if (mGroupList.size() <= 0)
            return 0;
        return getChildrenRosters(mGroupList.get(groupPosition).getGroupName()).size();
    }

    @Override
    public Group getGroup(int groupPosition) {
        return mGroupList.get(groupPosition);
    }

    @Override
    public Roster getChild(int groupPosition, int childPosition) {
        return getChildrenRosters(mGroupList.get(groupPosition).getGroupName()).get(childPosition);
    }

    @Override
    public long getGroupId(int groupPosition) {
        return groupPosition;
    }

    @Override
    public long getChildId(int groupPosition, int childPosition) {
        return childPosition;
    }

    @Override
    public boolean hasStableIds() {
        return true;
    }

    @Override
    public View getGroupView(int groupPosition, boolean isExpanded, View convertView, ViewGroup parent) {
        if (convertView == null) {
            convertView = mInflater.inflate(R.layout.contact_buddy_list_group, null);
        }
        TextView groupName = (TextView) convertView.findViewById(R.id.group_name);
        Group group = getGroup(groupPosition);

        groupName.setText(TextUtils.isEmpty(group.getGroupName()) ? mContext.getString(R.string.default_group) : group.getGroupName());
        TextView onlineNum = (TextView) convertView.findViewById(R.id.online_count);
        onlineNum.setText(group.getMembers());
        ImageView indicator = (ImageView) convertView.findViewById(R.id.group_indicator);
        if (isExpanded)
            indicator.setImageResource(R.drawable.indicator_expanded);
        else
            indicator.setImageResource(R.drawable.indicator_unexpanded);
        // 必须使用资源Id当key(不是资源id会出现运行时异常),android本意应该是想用tag来保存资源id对应组件。
        // 将groupPosition,childPosition通过setTag保存,在onItemLongClick方法中就可以通过view参数直接拿到了
        convertView.setTag(R.id.xxx01, groupPosition);
        convertView.setTag(R.id.xxx02, -1);
        return convertView;
    }

    @Override
    public View getChildView(int groupPosition, int childPosition, boolean isLastChild, View convertView, ViewGroup parent) {
        final Roster roster = getChild(groupPosition, childPosition);
        int presenceMode = Integer.parseInt(roster.getStatusMode());
        ViewHolder holder;
        if (convertView == null || convertView.getTag(R.drawable.qq_icon + presenceMode) == null) {
            LogUtil.i("liweiping", "new  child ");
            holder = new ViewHolder();
            convertView = mInflater.inflate(R.layout.contact_list_item_for_buddy, parent, false);
            holder.headView = (ImageView) convertView.findViewById(R.id.icon);
            holder.statusView = (ImageView) convertView.findViewById(R.id.stateicon);
            holder.nickView = (TextView) convertView.findViewById(R.id.contact_list_item_name);
            holder.onlineModeView = (ImageView) convertView.findViewById(R.id.online_mode);
            holder.statusMsgView = (TextView) convertView.findViewById(R.id.contact_list_item_state);
            convertView.setTag(R.drawable.qq_icon + presenceMode, holder);
            convertView.setTag(R.string.app_name, R.drawable.qq_icon + presenceMode);
        } else {
            LogUtil.i("liweiping", "get child form case");
            holder = (ViewHolder) convertView.getTag(R.drawable.qq_icon + presenceMode);
        }

        if(roster.getAlias() == null || "".equals(roster.getAlias().trim())){
            holder.nickView.setText(roster.getJid());
        }else{
            holder.nickView.setText(Html.fromHtml(""+roster.getAlias()+""));
        }

        holder.statusMsgView.setText(TextUtils.isEmpty(roster.getStatusMessage()) ? mContext.getString(R.string.status_offline) : roster.getStatusMessage());
        setViewImage(holder.onlineModeView, holder.headView, holder.statusView, roster.getStatusMode());

        convertView.setTag(R.id.xxx01, groupPosition);
        convertView.setTag(R.id.xxx02, childPosition);
        if(!mXmppService.isAuthenticated()){
            ToastUtil.showShort(mContext,"网络正在连接中...");
            return convertView;
        }
        VCard vCard = mXmppService.getUserAvatarByName(roster.getJid());
        vCard.getAvatar();
        byte[] userAvatarByte = vCard.getAvatar();
        if (userAvatarByte == null) {
            holder.headView.setImageResource(R.drawable.login_default_avatar);
        }else{
            Drawable userAvatar = ImageTools.byteToDrawable(vCard.getAvatar());
            holder.headView.setImageDrawable(userAvatar);
        }
        holder.headView.setOnClickListener(new View.OnClickListener() {
            @Override
            public void onClick(View v) {
                Intent intent = new Intent();
                intent.setClass(mContext,FriendInfoActivity.class);
                //intent.putExtra(FriendInfoActivity.FRIEND_JID_KEY,"admin@192.168.56.1");
                intent.putExtra(FriendInfoActivity.FRIEND_JID_KEY,roster.getJid());
                mContext.startActivity(intent);
            }
        });
        return convertView;
    }

    static class ViewHolder {
        ImageView headView;
        TextView nickView;
        ImageView statusView;
        ImageView onlineModeView;
        TextView statusMsgView;

    }

    protected void setViewImage(ImageView online, ImageView head, ImageView v, String value) {
        int presenceMode = Integer.parseInt(value);
        int statusDrawable = getIconForPresenceMode(presenceMode);
        if (statusDrawable == -1) {
            v.setVisibility(View.INVISIBLE);
            head.setImageResource(R.drawable.login_default_avatar_offline);
            online.setImageDrawable(null);
            return;
        }
        head.setImageResource(R.drawable.login_default_avatar);
        online.setImageResource(R.drawable.terminal_icon_ios_online);
        v.setImageResource(statusDrawable);

    }

    private int getIconForPresenceMode(int presenceMode) {
        return StatusMode.values()[presenceMode].getDrawableId();
    }

    @Override
    public boolean isChildSelectable(int groupPosition, int childPosition) {
        return true;
    }

    public class Group {
        private String groupName;
        private String members;

        public String getGroupName() {
            return groupName;
        }

        public void setGroupName(String groupName) {
            this.groupName = groupName;
        }

        public String getMembers() {
            return members;
        }

        public void setMembers(String members) {
            this.members = members;
        }

    }

    public class Roster {
        private String jid;
        private String alias;
        private String statusMode;
        private String statusMessage;

        public String getJid() {
            return jid;
        }

        public void setJid(String jid) {
            this.jid = jid;
        }

        public String getAlias() {
            return alias;
        }

        public void setAlias(String alias) {
            this.alias = alias;
        }

        public String getStatusMode() {
            return statusMode;
        }

        public void setStatusMode(String statusMode) {
            this.statusMode = statusMode;
        }

        public String getStatusMessage() {
            return statusMessage;
        }

        public void setStatus_message(String statusMessage) {
            this.statusMessage = statusMessage;
        }

    }
}

redpajama_set_name: RedPajamaGithub


text:
McLaren P1 to make debut at Paris Motor Show
10:10 PM PST - 9/18/2012 Written By: McLaren Automotive
Photography by: McLaren Automotive
2014 McLaren P1 Front 3Q Exterior View Source McLaren Automotive
McLaren Automotive will use its first ever international motor show appearance to preview its next generation ultimate supercar – the McLaren P1 – which takes much of its technological and spiritual inspiration from the company's Racing division. The McLaren P1 has one simple goal: to be the best driver's car in the world on road and track.
At the Paris Motor Show, Mondial de l'Automobile 2012, the McLaren P1 is previewed as a design study. Next year a production version, which the company aims to put on sale within 12 months, will be revealed.
'The McLaren P1 will be the result of 50 years of racing and road car heritage,'says McLaren Automotive Executive Chairman Ron Dennis. 'Twenty years ago we raised the supercar performance bar with the McLaren F1 and our goal with the McLaren P1 is to redefine it once again.'
'Our aim is not necessarily to be the fastest in absolute top speed but to be the quickest and most rewarding series production road car on a circuit,'says McLaren Automotive Managing Director Antony Sheriff. 'It is the true test of a supercar's all round ability and a much more important technical statement. Our goal is to make the McLaren P1 the most exciting, most capable, most technologically advanced and most dynamically accomplished supercar ever made.'
When the McLaren P1 goes into production later next year, it will sit above the 12C and 12C Spider, in terms of both price and performance.
2013 McLaren 12C GT3 off to a winning start
McLaren GT kicked off the 2013 European GT season in style, with French rally-ace Sébastien Loeb claiming victory in the opening round of the FIA GT Series at Nogaro...
McLaren 12C GT3 confirmed eligible for Pirelli World Challenge
McLaren 12C GT3 has been confirmed as eligible for the Pirelli World Challenge (PWC), by the series organizers following a strong competitive debut season in Europe. This announcement means that the British-built racer is now able to compete in North America for the first time...
McLaren P1 the number cruncher
McLaren Automotive has released the final numbers, images and information relating to its phenomenal McLaren P1™ ahead of a global reveal in just a few days at the 83rd International Geneva Motor Show. ...

redpajama_set_name: RedPajamaCommonCrawl


text:
General Election: The people standing for the Liberal Democrats in South Gloucestershire
They have put forward their candidates for Filton and Bradley Stoke, Kingswood and Thornbury & Yate
Amanda CameronLocal democracy reporter
The Liberal democrats want to abolish the role of mayor in Bristol (Image: PA)
The Liberal Democrat party has selected its candidates to fight the next general election in South Gloucestershire.
The county is split into three constituencies: Filton and Bradley Stoke, Kingswood, and Thornbury and Yate.
Louise Harris will contest Filton and Bradley Stoke, Dine Romero will stand in Kingswood, and Claire Young will once again fight for Thornbury and Yate.
Council bin men could return to the streets as part of attempt to save £19.4million
The three women were selected in a vote by party members in each area.
So who are the three prospective parliamentary candidates?
Louise Harris, PCC for Filton and Bradley Stoke
The Liberal Democrats newest councillor, Louise Harris (centre), with her fellow councillors and campaign team (Image: Copyright Unknown)
Louise Harris represents Dodington ward on South Gloucestershire Council.
She became a councillor in October 2018 when she won 49 per cent of the vote in a by-election held following the death of former Dodington councillor Gloria Stephens.
Cllr Harris said: "It's a great honour to become the candidate for Filton and Bradley Stoke.
Bristol billboard ads for 'safe' Rizlas banned because people might think smoking is actually safe
"I'm looking forward to speaking about Lib Dem priorities and values in the area. We know that South Gloucestershire and the country have been let down by the Conservatives on education, the NHS, local services and Brexit, and I'm eager to listen to residents about their concerns."
Conservative MP Jack Lopresti has held the seat since 2010.
Dine Romero, PCC for Kingswood
Louise Harris will contest Filton and Bradley Stoke, Dine Romero will stand in Kingswood, and Claire Young will once again fight for Thornbury and Yate
Dine Romero is the leader of the Lib Dem group of councillors in Bath and North East Somerset where she represents Southdown ward.
Cllr Romero will be hoping to unseat Conservative MP Chris Skidmore, who has represented Kingswood since 2010.
She said: "The Kingswood constituency is an area with two stories.
Ombudsmen upholds mum's complaint about South Glos school catchment areas
"There are areas of new development here with a commuting population who will be feeling very nervous about their jobs as we approach Brexit day, and there is another group living with deprivation in their community who want answers to Conservative austerity. The Lib Dems demand better than Brexit, which will only make that struggle worse."
Claire Young, PCC for Thornbury and Yate
Thornbury and Yate Liberal Democrat candidate, Claire Young
The party announced Claire Young, Westerleigh councillor, as their candidate for Thornbury and Yate last month.
Now leader of the Liberal Democrat group on South Gloucestershire Council, Cllr Young contested the seat in the last general election but was unsuccessful.
She said: "I'm delighted to stand alongside a team of talented women for the Lib Dems for the second election in a row.
"Voting Lib Dem here is a positive choice against the usual disappointing palate of bland politicos that will fill the Conservative and Labour tickets.
Developer submits plans for nearly 400 homes to north of Bristol
"Across our area, people are starting to demand better from Westminster, and I know Louise and Dine can provide it."
Conservative MP Luke Hall has represented Thornbury and Yate since May 2015.
The next general election is not due to take place until May 2022.
Filton


These assorted sample packages are perfect for small projects!
Sorry, we are currently sold out of 'SAMPLES- Rug fabric linen 4'. Please check back later.
Sorry, we are currently sold out of 'SAMPLES- map fabric vintage document- 2'. Please check back later.
Sorry, we are currently sold out of 'SAMPLE- Watercolor floral fabric linen-3'. Please check back later.
SAMPLE- Tropical floral fabric watercolor blue 39"
Sorry, we are currently sold out of 'SAMPLE- Tropical floral fabric watercolor blue 39"'. Please check back later.


Allcocks Outdoor Store provides a huge selection of essential Coarse Fishing accessories. Our range offers everything that you could possibly require for a day of Coarse Fishing. Choose from our selection of fishing floats, rig tubes, bait needles, bait pouches, bait buckets, catapults and much more.
With coarse fishing accessories from high quality fishing brands including Drennan, Browning, Guru, 30 Plus, Bait-Tech, Dinsmores, Polaris, Dynamite Baits, Middy, Seymo and many more; you can feel assured that you are purchasing the best coarse fishing products at Allcocks Outdoor Store.


text:
Working at UB >
Need to Know >
RENEW lecture to focus on El Niño, climate change
El Niño and climate change will be the topic of a RENEW Innovation Lecture on June 14.
The lecture, given by UB alumnus Michael McPhaden, senior scientist at NOAA's Pacific Marine Environmental Laboratory in Seattle, will take place at 11 a.m. in the Honors College, 107 Capen Hall, North Campus.
It is free and open to the UB community.
McPhaden, an expert in large-scale tropical ocean dynamics, ocean-atmosphere interactions and the ocean's role in climate, will discuss the 2015-16 El Niño. A surprisingly intense event, it rivaled the 1997-98 El Niño — the strongest on record — in its magnitude and impact.
In 2015-16, El Niño-related drought, flooding, extreme weather and wild fires affected far-reaching parts of the globe, with consequences for agriculture, power generation, economic development and human health.
In his talk, McPhaden will describe the evolution of the 2015-16 El Niño, the physical mechanisms that gave rise to it, how it compared to previous El Niño events and how well it was predicted by various forecasting centers. He also will address the question of whether anthropogenic greenhouse gas forcing is having an effect on El Niño.
A 1973 graduate of UB with a BS in physics and PhD in physical oceanography from the Scripps Institution of Oceanography, McPhaden has been involved for more than 35 years in developing ocean observing systems for climate research and forecasting, most notably the Tropical Atmosphere Ocean moored buoy array in the Pacific for studies of El Niño and the Southern Oscillation.
A past president of the American Geophysical Union, he has published nearly 300 articles in the refereed scientific literature and is one of the most highly cited authors on the topic of El Niño.
McPhaden shared the Nobel Peace Prize in 2007 with Al Gore and other participants of the Intergovernmental Panel on Climate Change, an international body for assessing the science related to climate change.


Do we need an art plan for Vancouver's West End?
Well, that's not an uncommon view outside our community. We've all encountered it from time to time, and we've all learned by rote the counter argument around heterosexual artistic expression being so omnipresent that nobody even notices.
"No guy-on-girl hand-holding or kissing, no . . ." — at which point the conversation dissolved into laughter.
Of course art by any minority artists is going to reflect the lives and experiences and dreams, fantasies and fears of those artists. In the West End the queer community and a vibrant art scene have always been deeply interconnected.
"It would take a very concerted effort to deliberately exclude queer arts and artists to have us not involved in any planning for the West End," Holman also noted.
The West End Art Plan had its beginnings seven years ago when West End resident Satomi Hirano saw something in a report about the arts in Vancouver that stuck with her.
So when Hirano attended one of the open house events leading up to the November 2013 adoption of the West End Community Plan, a 30-year master plan for the neighbourhood, she stood up to ask a question that launched a passionate community conversation.
Her question caught the ear of Stephen Regan, executive director of the West End Business Improvement Association, who offered to help her open a dialogue with West End businesses and residents about what could be done to support the arts in the area.
After all, the West End is one of Vancouver's most artful neighbourhoods, with some 4,000 of its 45,000 residents employed in the arts, culture and heritage sector.
With grants from Gordon Neighbourhood House and the Vancouver Foundation, WEArts has led several arts projects and, since February, has hosted three community forums facilitated by Art For Social Change's Judith Marcuse. Participants discussed the possibilities for a West End community richer than ever in cultural and artistic endeavours, venues and activities.
The final outcome of these consultations will be a West End Art Plan, to be presented to Vancouver city council this month to hopefully help inform the implementation of the West End Community Plan approved in 2013.
Among the more than 300 individual West Enders who have participated in the process, high priority has been given to the need for a dedicated arts centre (with longing eyes cast in the direction of the vacant Gabriola Mansion on Davie Street), more local business support in the form of pop-up galleries in vacant retail storefronts, greater use of public spaces such as the soon-to-be permanent Bute Street Plaza and the Alexandra Park Bandstand, and affordable studio, rehearsal, and live-work spaces for artists.
The queer community has been well represented throughout the process, with the organizing team meetings taking place directly across the hall from the Queer Arts Festival (QAF) office in Gordon Neighbourhood House, and that group has been involved from the very beginning.
Since then almost every queer-identified cultural and business organization with a West End presence has had a hand in the process. In addition to Holman, Iwassa, and Landon Krentz of QAF, the Vancouver Pride Society, OUTtv, the Vancouver Men's Chorus, the LOUD Foundation, and community leaders such as Barb Snelgrove and MLA Spencer Chandra Herbert have all engaged in the discussions.
If adopted to help inform the overall West End Community Plan, there will be a lot more work to be done in making the plan's vision a reality. From big picture work with city council and various civic government departments to make the necessary event and activity permits and zoning applications happen, to getting individual West End businesses and community organizations all on the same page, and hands-on community organizing to provide the catalyst for numerous initiatives, WEArts seems poised to provide the leadership the community will need.
If the West End Art Plan is embraced, and I hope it will be, it will be a clear signal from city council that the City of Vancouver is ready and willing to work with the community to fill in the spaces between the mushrooming towers of glass and steel with vibrant cultural expressions.
Clearly the queer community will be in the thick of those expressions, as it always has been where art, business, and life in the West End intersect.
Editor's note: This article was corrected on July 17, 2015 to reflect that, if accepted, the West End Arts Plan may help inform the implementation of the 2013 West End Community Plan but would not be adopted as an addition to the plan.


A group dedicated to studying and actively sharing horticulture history and exploring herb use, the Pennsylvania Heartland Herb Society is pleased to offer two $1,500 scholarships this year. These scholarships will be awarded to two students active within the field of horticulture or a related study. They will be awarded to students living in the Heartland area, which includes: Berks, Montgomery, Chester, York, Schuylkill, Lancaster, Columbia, Lehigh and Lebanon counties. Applicants must be third or fourth year students in the study of horticulture or a related field. Click here for details on how to apply.


text:
Stocks close lower on Wall Street as rally momentum cools
by: DAMIAN J. TROISE and ALEX VEIGA, AP Business Writers
(AP) — A sell-off on Wall Street left stocks broadly lower Thursday, giving back some of the market's gains from a three-day winning streak.
The S&P 500 fell 0.7%, with more than three-fourths of the companies in the benchmark index closing lower. The tech-heavy Nasdaq composite fell 1.7%, while the Dow Jones Industrial Average slipped less than 1 point.
Small-company stocks fell more than the rest of the market, sending the Russell 2000 index 2.3% lower. Roughly three stocks fell for every one that rose on the New York Stock Exchange.
The pullback follows a 3.6% gain for the S&P 500 index over the first three days of the week, largely in response to easing worries about the omicron variant of the COVID-19 virus. That marked an about-face for stocks following two weeks of losses over concerns about rising inflation and the coronavirus potentially crimping economic growth.
Investors welcomed reports this week of early indications suggesting the omicron variant may be less dangerous than delta, including word from Pfizer that its lab tests suggest the drugmaker's COVID-19 boosters provide protection against the new strain.
"Today, because of that, folks are taking a little bit of a breather to gauge other information that could suggest a more sustained direction for the market, particularly on the economic data front," said Greg Bassuk, CEO of AXS Investments.
The S&P 500 fell 33.76 points to 4,667.45. The Dow slipped less than 1 point to 35,754.69. The Nasdaq fell 269.62 points to 15,517.37. The Russell 2000 gave up 51.50 points to 2,220.71. Every major index is still on track for a weekly gain.
Technology stocks and a mix of retailers and other companies that rely on direct consumer spending weighed on the S&P 500 the most. Chipmaker Nvidia fell 3.4%, while Tesla slid 6.1% for the biggest drop in the index.
Travel-related companies slipped after spending the last few days gaining ground. Carnival fell 1.7% and United Airlines fell 1.8%.
Bond yields fell slightly. The yield on the 10-year Treasury fell to 1.49% from 1.51% late Wednesday.
Energy futures closed mostly lower. The price of U.S. crude oil fell 2% and helped pull energy stocks lower. Devon Energy fell 4%.
Health care companies rose. CVS Health climbed 4.5% after raising its dividend and issuing a solid forecast. Pfizer, which has been touting the potential benefits of a vaccine booster against the latest COVID-19 variant, rose 1.3%.
Investors received an encouraging update on job market's recovery. The Labor Department reported that the number of Americans applying for unemployment benefits plunged last week to the lowest level in 52 years.
The employment market's recovery has been a key focus for Wall Street while it gauges the strength of the economy as it moves past the virus pandemic. Rising inflation has been another focus, and investors will get an update Friday when the Labor Department releases its Consumer Price Index for November.
The latest inflation data comes ahead of the Federal Reserve's two-day meeting of policymakers next week. Rising inflation has prompted the central bank to speed up the pace at which it trims its bond purchases, which have helped keep interest rates low. That has raised concerns that the Fed will raise its benchmark interest rates next year sooner than expected.
Up to 6 Tornadoes Hit Florida


Do I really need a termite monitoring system if termites aren't present in my home?
Termite prevention is essential for all homeowners. Waiting until termites actually strike to take action to get rid of them is one of the biggest termite control mistakes a homeowner can make. Your home is simply too important, and the potential damages are too great, for a cross-your-fingers-and-wait strategy when it comes to termite control.
Advance Termite Monitoring is a professional termite monitoring system that watches over your home 24 hours a day and lets your pest professional check regularly to make sure termites are not present.
Advance Termite Monitoring stations with termite inspection cartridges are strategically installed around your home. These cartridges contain active-ingredient-free Puri-Cell® monitoring tablets that termites find even more appetizing than wood.
If termites do show up at your home, the termite monitoring system can reveal their presence to your pest management professional, who will then work with you to determine the best next-step termite prevention and termite treatment strategies for your home and circumstances.


One of the most beautiful section of the LMT (Lebanon Moutain Trail) to my opinion, the tracks who goes from Aaquoura to Afqa is really pleasant and easy. You will enjoy stunning views on Nahr Ibrahim Valley (Adonis Valley) on the ridge of the mountain. As I said, the path is quiet easy to follow and not technical at all. Although It is around 20 km so you need to be in quiet good shape. The village of Aaqoura is famous for its 44 religious place so give it a stop to have a visit ! About Afqa, the village is famous for its waterfall who is also the source of Nahr Ibrahim river.


text:
Q: What component is this? (photo) My PC powered off out of the blue one night and when I opened it to look for a burning smell I didn't notice any, so I thought it might be due to a power surge and tried to boot up the PC again with the cabinet open and that is when I saw a yellow spark fly out from the graphic card. I checked my PowerColor HD 7970 graphic card and I noticed a burnt out component on the back side.
I've marked the burnt out component in the cropped photo below.

Initially I thought it was a Surface Mount Capacitor because of the 'C' in the label C610. So tried to contact a computer repairs shop and they said that it wasn't a capacitor but I'm not sure if the guy knew what it actually was.
Can someone help me figure out what type of a component it is? I'm assuming C610 is the same as C618 or C623 because it looks like they are the same size.
P.S. My PC boots up fine using the on board graphic card it has so there is not damage to the motherboard I think.
Also I have a multi-meter available in case you want me to test something and report back.
Update : The IC 8510 301-24 U1216 below the burnt capacitor in the photo is dead too.

A: Well, according to the picture it looks like you have 5 examples of the circuit side by side from left to right - they all interface with identical chips (U1216 written on them amongst other similar identifiers). I've marked each circuit with a white box: -

So, get someone to remove one of the components that should be identical and get them to measure it to confirm it is a capacitor and buy a replacement.

A: Not sure why the guy in the computer repair shop would claim it's something other than a capacitor - it is obviously a capacitor, for three reasons:

*

*It's named Cxxx

*It's placed in parallel with a lot of other capacitors

*The placement indicates that it belongs to the power supply section

As for the value and voltage rating, that's more difficult. There are minor differences between each section. With any luck you will find a recommended value from the datasheet of the controller IC. It's unlikely to be critical.
In fact, it would not surprise me if the graphics card still works if you clean the soot off.

redpajama_set_name: RedPajamaStackExchange


text:
Q: Installing Ruby on Rails from Source - cannot load such file -- openssl I am on a Mac, using Lion. I am configuring my system for Ruby on Rails development but I ran into some issues. Instead of using brew or other shortcuts I want to configure Ruby on Rails from source. So, here is what I did.
Installed Ruby 2.0

*

*Downloaded the source from the Ruby website

*Compiled it by running the following code:
./configure --prefix=/Users/user/Applications/ruby2
make
make install

*And made sure the $PATH file is updated to point to /Users/user/Applications/ruby2/bin
So, I am able to call ruby -v or if I do which ruby it does point to my custom compiled version of Ruby.
Installed Node.js

*

*Downloaded the source from the main website

*Compiled it by running the following code:
./configure --prefix=/Users/user/Applications/nodejs
make
make install

*And made sure the $PATH file is updated to point to /Users/user/Applications/nodejs/bin
So, I am able to call node -v or if I do which node it does point to my custom compiled version of Ruby.
I also did the same steps for openssl and it is also accessible from the console or if I do which openssl it points to /Users/user/Application/openssl/bin
But still when I execute gem install rails I still get the following error:
ERROR:  Loading command: install (LoadError)
    cannot load such file -- openssl
ERROR:  While executing gem ... (NoMethodError)
    undefined method `invoke_with_build_args' for nil:NilClass

Any idea why?
System Specs

*

*Mac Lion 10.8.4

*OpenSSL 1.0.1e 11 Feb 2013

*ruby 2.0.0p291

*Nodejs v0.10.15

A: I managed to solve the problem by doing the following. The main problem was the step I followed to compile openssl itself.
Since I am on a 64 bit machine, I had to configure openssl by running the following command first
./configure --prefix=/Users/user/Applications/openssl darwin64-x86_64-cc
./make
./make install

And recompile ruby as such
./configure --prefix=/Users/user/Applications/ruby2 --with-openssl-dir=/Users/user/Applications/openssl
./make
./make install

Note: Even though while compiling ruby it might say... the option --with-openssl-dir is not valid or does not exist, ignore that.

A: I had very bad time with this ERROR.
Finally i done with it. There is only Once solution either you are with RVM or without RVM.
Make sure you have installed OpenSSL first BEFORE installing ruby.
First you should find where Ruby is:
whereis ruby

will list all the places where it exists on your system, then you can remove all them explicitly. Or you can use something like this:
rm -rf /usr/local/lib/ruby
rm -rf /usr/lib/ruby
rm -f /usr/local/bin/ruby
rm -f /usr/bin/ruby
rm -f /usr/local/bin/irb
rm -f /usr/bin/irb
rm -f /usr/local/bin/gem
rm -f /usr/bin/gem

THEN
sudo apt-get install zlib1g zlib1g-dev build-essential openssl libssl-dev libmysqlclient18 libmysqlclient-dev libyaml-dev curl git-core python-software-properties libpq-dev nodejs

apt-get -y update
apt-get -y install build-essential zlib1g-dev libssl-dev libreadline6-dev libyaml-dev
cd /tmp
wget http://cache.ruby-lang.org/pub/ruby/2.0/ruby-2.0.0-p247.tar.gz
tar -xvzf ruby-2.0.0-p247.tar.gz
cd ruby-2.0.0-p247/
./configure --prefix=/usr/local
make
make install

I hope this help you.


Presentation House Gallery is pleased to announce NEWS!, an exhibition at Satellite Gallery that takes an in-depth look at the news photography archives of The Vancouver Sun and Province newspapers. This unique collection holds a breadth of material that includes hundreds of thousands of photographs from the 1880s to the 1990s. The exhibition will trace the history of Vancouver through a selection of photographs and ephemeral material. It will reveal how news photography evolved dramatically over the past hundred years as pictures began to play a more important role in newspapers. Over the twentieth century, occasional illustrations were replaced by photographs, which dominated the pages of newspapers by the 1960s, when staff photographers were in abundance. Television and picture magazines such as LIFE also helped shift public understandings of current affairs from the written word to images.
NEWS! will explore the developments of photography as a medium. The range of pictures reveals many subjects and styles of photography: comic photo-ops, famous visitors, civic events, prominent politicians and anonymous citizens, disasters, scandals, and plenty of sports—a specialty of many staff photographers. The exhibition also includes material from the archive, and brings to light its intricate filing and indexing systems.
NEWS! is made possible with assistance from the The Vancouver Sun and Province newspapers.