diff --git a/DIS2015/Rare_decays/mchrzasz.log b/DIS2015/Rare_decays/mchrzasz.log
index 0b58e03..9433a71 100644
--- a/DIS2015/Rare_decays/mchrzasz.log
+++ b/DIS2015/Rare_decays/mchrzasz.log
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diff --git a/SM@LHC/mchrzasz.synctex.gz b/SM@LHC/mchrzasz.synctex.gz
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+\def\ATImPH {\ensuremath{A_{\mathrm{T,PR}}^{\mathrm{Im}}}\xspace}
+\def\ATRePH {\ensuremath{A_{\mathrm{T,PR}}^{\mathrm{Re}}}\xspace}
+\def\FLPH {\ensuremath{F_{\mathrm{L,PR}}}\xspace}
+\def\ATDKG {\ensuremath{A_{\mathrm{T,\Kstarz \gamma}}^{(2)}}\xspace}
+\def\ATImKG {\ensuremath{A_{\mathrm{T,\Kstarz \gamma}}^{\mathrm{Im}}}\xspace}
+\def\ATReKG {\ensuremath{A_{\mathrm{T,\Kstarz \gamma}}^{\mathrm{Re}}}\xspace}
+\def\FLKG {\ensuremath{F_{\mathrm{L,\Kstarz \gamma}}}\xspace}
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+\def\ATRe {\ensuremath{A_{\mathrm{T}}^{\mathrm{Re}}}\xspace}
+
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+
+
+\newcommand{\disp}{\displaystyle}
+\def\be{\begin{equation}}
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+\def\ea{\end{eqnarray}}
+\def\d{\partial}
+\def\l{\left(}
+\def\r{\right)}
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+\def\ra{\rangle}
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+\def\Br{{\rm Br}}
+
+\def\ARROW{{\color{JungleGreen}{$\Rrightarrow$}}\xspace}
+
+\newcommand\textref[1]{%
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+
+\author{ {\fontspec{Trebuchet MS}Marcin Chrz\k{a}szcz} (Universit\"{a}t Z\"{u}rich, IFJ PAN)}
+\institute{UZH, IFJ PAN}
+\title[Overview of recent experimental results in flavour physics]{Overview of recent experimental results in flavour physics}
+\date{25 September 2014}
+
+
+\begin{document}
+\tikzstyle{every picture}+=[remember picture]
+
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+{
+\setbeamertemplate{sidebar right}{\llap{\includegraphics[width=\paperwidth,height=\paperheight]{bubble2}}}
+\begin{frame}[c]%{\phantom{title page}}
+\begin{center}
+\begin{center}
+ \begin{columns}
+ \begin{column}{0.75\textwidth}
+ \flushright\fontspec{Trebuchet MS}\bfseries \LARGE {Overview of recent experimental results in flavour physics}
+ \end{column}
+ \begin{column}{0.02\textwidth}
+ {~}
+ \end{column}
+ \begin{column}{0.23\textwidth}
+ % \hspace*{-1.cm}
+ \vspace*{-3mm}
+ \includegraphics[width=0.6\textwidth]{lhcb-logo}
+ \end{column}
+
+ \end{columns}
+\end{center}
+ \quad
+ \vspace{3em}
+\begin{columns}
+\begin{column}{0.44\textwidth}
+\flushright \vspace{-1.8em} {\fontspec{Trebuchet MS} \Large Marcin ChrzÄ…szcz\\\vspace{-0.1em}\small \href{mailto:mchrzasz@cern.ch}{mchrzasz@cern.ch}}
+
+\end{column}
+\begin{column}{0.53\textwidth}
+\includegraphics[height=1.3cm]{uzh-transp}{~}{~}
+\includegraphics[height=1.1cm]{ifj.png}
+\end{column}
+\end{columns}
+
+\vspace{1em}
+ \footnotesize\textcolor{gray}{on behalf of the LHCb collaboration,\\ Universit\"{a}t Z\"{u}rich, \\ Institute of Nuclear Physics, Polish Academy of Science}\normalsize\\
+\vspace{0.5em}
+
+ \textcolor{normal text.fg!50!Comment}{Pittsburgh, 3-6 May 2016}
+\end{center}
+\end{frame}
+}
+
+
+
+
+\begin{frame}{Flavour Physics, WHAT, WHY HOW?}
+
+ \begin{minipage}{\textwidth}
+\begin{footnotesize}
+{~}\\
+\ARROW WHAT: Quarks and leptons exists in 6 ''flavors'' (u,c,t,d,s,b) and (e,$\mu$, $\tau$, $\nu_e$, $\nu_{\mu}$, $\nu_{\tau}$).\\
+\ARROW WHY:
+\begin{itemize}
+\item Flavour is the heart of SM. It involves $22$ from $28$ free parameters, like masses mixing and CP violation.
+\item Flavor physics loop processes (box and penguins) are sensitive to energy scales well beyond the ones of the accelerators, thanks to virtual contributions.
+\end{itemize}
+\begin{center}
+\includegraphics[width=0.8\textwidth]{images/mglass.png}
+\end{center}
+\ARROW HOW:
+\begin{itemize}
+\item Compare precise theoretical predictions with precise experimental measurements.
+\item LHCb, Belle, BaBar, ATLAS, CMS, NA62, BESIII, neutrinos experiments,...
+\end{itemize}
+
+
+
+\end{footnotesize}
+\end{minipage}
+ \vspace*{2.cm}
+\end{frame}
+
+\begin{frame}{Introduction to flavor physics}
+
+ \begin{minipage}{\textwidth}
+\begin{footnotesize}
+{~}\\{~}\\
+\ARROW Masses and mixing of quarks have a common origin in the SM: The Yukawa interactions with the Higgs:
+\begin{align*}
+\mathcal{L}_{ \rm Yukawa}= - Y_{ij}^d \bar{Q^{\prime}}_{Li} \phi d^{\prime}_{Rj} - Y_{ij}^u \bar{Q^{\prime}}_{Ri} \phi u^{\prime}_{Rj}
+\end{align*}
+\ARROW The masses are generated using SSB by diagonalizing $Y$. The CKM matrix relats the mass eigenstates with the flavour eigenstates:
+\begin{align*}
+\begin{pmatrix}
+ d \\
+ s \\
+ b
+ \end{pmatrix}^{\prime}
+ =
+ \begin{pmatrix}
+ V_{ud} & V_{us} & V_{ub} \\
+ V_{cd} & V_{cs} & V_{cb} \\
+ V_{td} & V_{ts} & V_{tb}
+ \end{pmatrix}
+ \begin{pmatrix}
+ d \\
+ s \\
+ b
+ \end{pmatrix}^{ \rm phys}
+\end{align*}
+\ARROW The charge current interactions between quarks are proportional to the CKM matrix elements:
+\begin{columns}
+\column{3in}
+\begin{align*}
+\mathcal{L}_{CC}=-\frac{g}{\sqrt{2}} \bar{u} \gamma^{\mu}(1-\gamma^5)V_{CKM}d+...
+\end{align*}
+\column{2in}
+\includegraphics[width=0.85\textwidth]{images/in_thi9.png}
+\end{columns}
+
+
+\end{footnotesize}
+\end{minipage}
+ \vspace*{2.cm}
+\end{frame}
+
+\begin{frame}{CP violation}
+
+ \begin{minipage}{\textwidth}
+\begin{footnotesize}
+{~}\\{~}\\
+\ARROW The $3 \times 3$ CKM has build inside the CP violation:
+\begin{align*}
+V_{ij} \neq V_{ij}^{\ast}~~\Rightarrow~~(CP)\mathcal{L}_{CC} \neq \mathcal{L}^{\dag}
+\end{align*}
+\ARROW In the Wolfenstein parametrization the CKM matrix reads:
+\begin{align*}
+V_{CKM}=
+\begin{pmatrix}
+1-\lambda^2/2 & \lambda & A\lambda^3(\rho- i \eta)\\
+-\lambda & 1-\lambda^2/2 & A \lambda^2 \\
+A \lambda^3 (1-\rho - i \eta) & -A \lambda^2 & 1
+\end{pmatrix}
+\end{align*}
+\ARROW Strong hierarchy:
+
+\begin{columns}
+\column{2in}
+\includegraphics[width=0.9\textwidth]{images/ckm.jpg}
+\column{3in}
+\includegraphics[width=0.9\textwidth]{images/quarkmasses.png}
+\end{columns}
+
+
+\end{footnotesize}
+\end{minipage}
+ \vspace*{2.cm}
+\end{frame}
+
+
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}\frametitle{Why rare decays?}
+\begin{columns}
+\column{4in}
+\begin{itemize}
+\item In SM allows only the charged interactions to change flavour.
+\begin{itemize}
+\item Other interactions are flavour conserving.
+\end{itemize}
+\item One can escape this constrain and produce $\Pbottom \to \Pstrange$ and $\Pbottom \to \Pdown$ at loop level.
+\begin{itemize}
+\item This kind of processes are suppressed in SM $\to$~Rare decays.
+\item New Physics can enter in the loops.
+\end{itemize}
+\end{itemize}
+\begin{center}
+\includegraphics[scale=0.3]{images/lupa.png}
+\includegraphics[scale=0.3]{images/example.png}
+\end{center}
+\column{1.5in}
+\includegraphics[width=0.61\textwidth]{images/couplings.png}
+\end{columns}
+
+
+
+
+\end{frame}
+
+
+\begin{frame}{Searching for New Physics}
+ \begin{minipage}{\textwidth}
+\begin{footnotesize}
+{~}\\{~}\\
+\ARROW The fundamental questions:
+\begin{itemize}
+\item Why 3 generations? Why such hierarchy structure?
+\item Stability of the Higgs vacum? Dark Matter?
+\item Baryon asymmetry of the universe? CP in SM is to small!
+\end{itemize}
+\pause
+\ARROW Two ways to answer them:
+\begin{itemize}
+\item Direct searches: try to produce directly new real particles ''on-shell'', but we don’t
+know their mass or lifetime and we are limited by the center-of-mass energy of
+accelerator.
+\item Indirect searches: study the effect of “off-shell” (virtual) particles within quantum
+loop. Compare precise theoretical predictions with precise experimental measurements. Not limited by the center-of-mass energy of accelerator. It happened in the past:
+\begin{itemize}
+\item CP violation in the Kaon system: existence of $\Pbeauty$ and $\Ptop$ quarks.
+\item Lack of observation of $\PKs \to \mu \mu$: existence of $\Pcharm$ quark.
+\item Neutral weak currents: existence of $\PZ$ boson.
+\end{itemize}
+\item Very powerful tool!
+\end{itemize}
+\end{footnotesize}
+\end{minipage}
+ \vspace*{2.cm}
+\end{frame}
+
+
+
+\begin{frame}{Selected physics results:}
+ \begin{minipage}{\textwidth}
+\begin{footnotesize}
+{~}\\{~}\\
+\begin{itemize}
+\item Rare Decays
+\begin{itemize}
+\item $\PBs/ \PBd \to \Pmu \Pmu$
+\item $\PBd \to \PKstar \Pmu \Pmu$, $\PBs \to \Pphi \Pmu \Pmu$, $\PLambdab \to \PLambda \Pmu \Pmu$.
+\end{itemize}
+\item Tests of lepton universalities:
+\begin{itemize}
+\item $R_k=\mathcal{B}(\PBplus \to \PKplus \Pmu \Pmu) / \mathcal{B}(\PBplus \to \PKplus \Pe \Pe)$
+\item $R(\PD),~ R(\PDstar)$
+\end{itemize}
+\item $(g-2)_{\mu}$
+\item CP violation:
+\begin{itemize}
+\item $\gamma$ angle.
+\item CP violation in $\PBd $ and $\PBs$.
+\item CP violation in charm.
+\item CP violation in kaons.
+\item $V_{ub}$.
+\end{itemize}
+\end{itemize}
+
+
+\end{footnotesize}
+\end{minipage}
+ \vspace*{2.cm}
+\end{frame}
+
+
+
+
+
+\begin{frame}{Heavy flavor experiments}
+ \begin{minipage}{\textwidth}
+\begin{footnotesize}
+{~}\\{~}\\
+
+
+
+
+\end{footnotesize}
+\end{minipage}
+ \vspace*{2.cm}
+\end{frame}
+
+\begin{frame}
+\begin{center}
+\begin{Huge}
+Rare decays
+\end{Huge}
+\end{center}
+
+
+\end{frame}
+
+
+\begin{frame}\frametitle{Tools}
+\begin{itemize}
+\item \textbf{Operator Product Expansion and Effective Field Theory}
+\end{itemize}
+\begin{columns}
+\column{0.1in}{~}
+\column{1.2in}
+\begin{small}
+\begin{align*}
+H_{eff} = - \dfrac{4G_f}{\sqrt{2}} V V^{\prime \ast}\ \sum_i \left[\underbrace{C_i(\mu)O_i(\mu)}_\text{left-handed} +\underbrace{C'_i(\mu)O'_i(\mu)}_\text{right-handed}\right],
+\end{align*}
+\end{small}
+\column{1.8in}
+\begin{tiny}
+\begin{description}
+ \item[i=1,2] Tree
+ \item[i=3-6,8] Gluon penguin
+ \item[i=7] Photon penguin
+ \item[i=9.10] EW penguin
+ \item[i=S] Scalar penguin
+ \item[i=P] Pseudoscalar penguin
+ \end{description}
+
+\end{tiny}
+\end{columns}
+where $C_i$ are the Wilson coefficients and $O_i$ are the corresponding effective operators.
+\begin{center}
+\includegraphics[width=0.85\textwidth,height=3cm]{images/all.png}
+
+\end{center}
+
+
+\end{frame}
+
+
+
+
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}\frametitle{$\PBzero \rightarrow \Pmu^+ \Pmu^-$}
+\begin{columns}
+\column{3.2in}
+
+\begin{itemize}
+\item Clean theoretical prediction, GIM and helicity suppressed in the SM:
+\begin{itemize}
+\item $\mathcal{B}(\PBs \to \Pmuon \APmuon) = (3.65 \pm 0.23)\times 10^{-9}$
+\item $\mathcal{B}(\PBzero \to \Pmuon \APmuon) = (1.06 \pm 0.09)\times 10^{-10}$
+\end{itemize}
+\item Sensitive to contributions from scalar and pesudoscalar couplings.
+\item Probing: MSSM, higgs sector, etc.
+\item In MSSM: $\mathcal{B}(\PBs \to \Pmuon \APmuon) \sim \tan^6 \beta /m_A^4$
+\end{itemize}
+
+\column{1.5in}
+{~}
+\includegraphics[width=0.95\textwidth]{hql/bs2mumu1.png}\\
+\includegraphics[width=0.95\textwidth]{hql/bs2mumu2.png}\\
+\includegraphics[width=0.6\textwidth]{hql/higgspen.png}
+\end{columns}
+
+
+\end{frame}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}\frametitle{$\PBzero \rightarrow \Pmu^+ \Pmu^-$ searches}
+
+
+\begin{columns}
+\column{5in}
+
+\begin{itemize}
+\item Background rejection power is a key feature of rare decays $\rightarrow$ use multivariate classifiers (BDT) and strong PID.
+\end{itemize}
+\column{0.1in}{~}
+
+\end{columns}
+\begin{columns}
+\column{2.5in}
+\includegraphics[width=0.95\textwidth]{hql/BDT.png}
+
+\column{2.5in}
+
+\includegraphics[width=0.95\textwidth]{hql/mass.png}
+
+\end{columns}
+
+\begin{itemize}
+\item Normalize the BF to $\PBplus \to \PJpsi(\mu\mu) \PKplus$ and $\PBzero \to \PK \Ppi$.
+\end{itemize}
+\textref{ PRL 111 (2013) 101805}
+
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}\frametitle{$\PBzero \rightarrow \Pmu^+ \Pmu^-$ Results}
+
+
+
+\begin{columns}
+\column{2.in}
+\begin{itemize}
+\item Nov. 2012:
+\begin{itemize}
+\item First evidence $3.5\sigma$ for $B^0 \rightarrow \mu^+ \mu^-$. with $2.1~\rm fb^{-1}$.
+\end{itemize}
+\item Summer 2013:
+\begin{itemize}
+\item Full data sample: $3~\rm fb^{-1}$.
+\end{itemize}
+\end{itemize}
+\column{3.0in}
+
+\includegraphics[width=0.95\textwidth]{hql/mass2.png}
+
+\end{columns}
+\begin{itemize}
+\item Measured BF:\\ $\mathcal{B}(\PBs \to \Pmuon \APmuon) =(2.9^{+1.1}_{-1.0}(stat.)^{+0.3}_{-0.1}(syst.))\times 10^{-9}$
+\item $4.0 \sigma$ significance!
+\item $\mathcal{B}(\PBzero \to \Pmuon \APmuon) < 7 \times 10^{-10}$ at $95\%$ CL
+%\item \href{http://journals.aps.org/prl/abstract/10.1103/PhysRevLett.110.021801}{\color{blue} PRL 110 (2013) 021801 }
+\item \href{http://journals.aps.org/prl/abstract/10.1103/PhysRevLett.111.101805}{\color{blue} CMS result: PRL 111 (2013) 101805}
+\end{itemize}
+
+\textref{ PRL 110 (2013) 021801}
+\end{frame}
+
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}\frametitle{LHCb+CMS Combination}
+\begin{columns}
+\column{3in}
+\begin{large}
+\begin{center}
+$\mathcal{B}(\PBs \to \Pmuon \APmuon) =(2.8^{+0.7}_{-0.6} )\times 10^{-9}$\\
+$\mathcal{B}(\PBzero \to \Pmuon \APmuon) =(3.9^{+1.6}_{-1.4} )\times 10^{-10}$
+\end{center}
+\end{large}
+\column{2in}
+\includegraphics[width=0.95\textwidth]{images/nature.png}
+\end{columns}
+
+
+\includegraphics[width=0.95\textwidth]{hql/bs2mumu_comb.png}
+\ARROW $2.3~\sigma$ compatibility with SM!
+
+
+\textref{Nature 522 (2015) 68}
+
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}\frametitle{ATLAS enters the game}
+\begin{columns}
+\column{3in}
+\begin{itemize}
+\item $\mathcal{B}(\PBs \to \Pmuon \APmuon) =0.9^{+1.1}_{-0.8} \times 10^{-9}$\\
+\item $\mathcal{B}(\PBzero \to \Pmuon \APmuon) <4.2 \times 10^{-10} $ at $95~\rm CL$
+\end{itemize}
+
+\includegraphics[width=0.95\textwidth]{images/atlas2.png}
+\column{2in}
+\includegraphics[width=0.95\textwidth]{images/atlas.png}\\
+\includegraphics[width=0.95\textwidth]{images/atlas3.png}
+
+\end{columns}
+
+
+
+\textref{arXiv:1604.04263}
+
+\end{frame}
+
+
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{$\PBd \to \PKstar \Pmu \Pmu$}
+\begin{footnotesize}
+
+{~}\\
+\begin{minipage}{\textwidth}
+\ARROW The decay of $\PBd \to \PKstar \Pmu \Pmu$ has number of angular observables that are sensitive to different Wilson coefficients: $C_7^{(\prime)},~C_9^{(\prime)},~C_{10}^{(\prime)}$.\\
+\ARROW The complete angular expression is given by:
+\iffalse
+{\tiny{
+\begin{align*}
+\label{dist}
+ \dfrac{1}{d \Gamma /dq^2} \frac{d^4\Gamma}{dq^2\,d\!\cos\theta_K\,d\!\cos\theta_l\,d\phi} = \frac9{32\pi}[ \frac{3}{4}(1- {\color{red}{F_L}} \sin^2\theta_K + {\color{red}{F_L}} \cos^2\theta_K + \\ \frac{1}{4} (1-{\color{red}{F_L }} )\sin^2\theta_K \cos 2\theta_l \\ - {\color{red}{F_L}} \cos^2\theta_K \cos 2\theta_l + {\color{red}{S_3}} \sin^2\theta_K \sin^2\theta_l \cos 2\phi + {\color{red}{S_4}} \sin 2\theta_K \sin 2\theta_l \cos\phi + {\color{red}{S_5}} \sin 2\theta_K \sin\theta_l \cos\phi \\ + ({\color{red}{S_{6s}}} \sin^2\theta_K + {\color{red}{{S_{6c}}}} \cos^2\theta_K) \cos\theta_l + {\color{red}{S_7}} \sin 2\theta_K \sin\theta_l \sin\phi + {\color{red}{S_8}} \sin 2\theta_K \sin 2\theta_l \sin\phi + {\color{red}{S_9}} \sin^2\theta_K \sin^2\theta_l \sin 2\phi ]
+\end{align*}
+}}
+\fi
+\begin{center}
+\includegraphics[width=0.85\textwidth]{images/angles4.png}
+\end{center}
+\ARROW Furthermore, one can construct a form factor free observables:
+\begin{align*}
+P_5^{\prime}=\frac{S_5}{F_L(1-F_L)}
+\end{align*}
+\ARROW Analysis performed with 3 methods:\begin{itemize}
+\item Likelihood fit.
+\item Method of moments.
+\item Amplitudes fit.
+\end{itemize}
+
+
+\end{minipage}
+\vspace*{2.1cm}
+ \vspace*{2.1cm}
+ \end{footnotesize}
+\textref{JHEP, 1305:137, (2013)}
+
+\end{frame}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{$\PBd \to \PKstar \Pmu \Pmu$ results}
+ \begin{minipage}{\textwidth}
+ \begin{center}
+ \includegraphics[width=0.65\textwidth]{images/p5pbelle.png}\\
+ \end{center}
+
+\begin{itemize}
+\item Tension with $3~\invfb$ gets confirmed!
+\item two bins both deviate by $2.8~\sigma$ from SM prediction.
+\item Result compatible with previous results and Belle!
+\item SM: \href{http://arxiv.org/abs/1407.8526}{\color{blue}JHEP12(2014)125}
+\end{itemize}
+
+
+\end{minipage}
+ \vspace*{2.1cm}
+ \textref{arxiv:1604.04042}
+
+\end{frame}
+
+
+
+
+
+
+
+
+
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
+
+
+\begin{frame}{$\PBd \to \PKstar \Pmu \Pmu$ results}
+{~}
+\begin{footnotesize}
+ \begin{minipage}{\textwidth}
+
+\only<3>
+{
+\ARROW Method of Moments allowed us to measure for the first time a new observable:
+}
+
+\begin{center}
+\only<1>{
+\includegraphics[angle=-90,width=0.49\textwidth]{images/compare_FLPad.pdf}
+\includegraphics[angle=-90,width=0.49\textwidth]{images/compare_S3Pad.pdf}\\
+\includegraphics[angle=-90,width=0.49\textwidth]{images/compare_S4Pad.pdf}
+\includegraphics[angle=-90,width=0.49\textwidth]{images/compare_S5Pad.pdf}
+}
+\only<2>{
+\includegraphics[angle=-90,width=0.49\textwidth]{images/compare_AFBPad.pdf}
+\includegraphics[angle=-90,width=0.49\textwidth]{images/compare_S7Pad.pdf}\\
+\includegraphics[angle=-90,width=0.49\textwidth]{images/compare_S8Pad.pdf}
+\includegraphics[angle=-90,width=0.49\textwidth]{images/compare_S9Pad.pdf}
+}
+\only<3>{
+\includegraphics[angle=-90,width=0.75\textwidth]{images/S6cPad.pdf}\\
+
+\begin{flushleft}
+\ARROW LHCb also measured the CP asymmetries with Method of Moments and the likelihood fit that are consistent with SM
+\end{flushleft}
+
+}
+
+\end{center}
+
+\end{minipage}
+\end{footnotesize}
+ \textref{JHEP 02 (2016) 104}
+
+ \vspace*{2.1cm}
+\end{frame}
+
+
+
+
+
+
+
+\begin{frame}{Compatibility with SM}
+{~}
+
+ \begin{minipage}{\textwidth}
+
+\begin{columns}
+\column{0.1in}
+{~}
+\column{2in}
+\ARROW Use \texttt{EOS} software package to test compatibility with SM.\\
+\ARROW Perform the $\chi^2$ fit to the measured:
+\begin{center}
+\begin{align*}
+F_L, A_{FB}, S_{3,..., 9} .
+\end{align*}
+\end{center}
+\ARROW Float a vector coupling: $\Re(C_9)$.\\
+\ARROW Best fit is found to be $3.4~\sigma$ away from the SM.
+
+
+\column{3in}
+\begin{align*}
+\Delta \Re (C_9) \equiv \Re(C_9)^{{\rm fit}} - \Re(C_9)^{{\rm SM}} = -1.03
+\end{align*}
+\includegraphics[angle=-90,width=0.95\textwidth]{images/wilsonchi2.pdf}
+\end{columns}
+
+
+
+\end{minipage}
+ \textref{JHEP 02 (2016) 104}
+
+ \vspace*{2.1cm}
+\end{frame}
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{BF of $\PB \to \PKstar^{\pm} \Pmu \Pmu$}
+{~}
+\includegraphics[width=0.5\textwidth]{images/ksmumu_BF.png}
+\includegraphics[width=0.5\textwidth]{images/kmumu_BF.png}
+
+\begin{center}
+\begin{columns}
+
+\column{0.4\textwidth}
+\begin{itemize}
+\item Despite large theoretical errors the results are consistently smaller than SM prediction.
+\end{itemize}
+\column{0.6\textwidth}
+\includegraphics[width=0.87\textwidth]{images/bukst_BF.png}
+
+
+\end{columns}
+
+
+
+
+
+
+
+\end{center}
+ \textref{JHEP 07 (2012) 133}
+
+ \vspace*{2.1cm}
+\end{frame}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{BF of $\PBs \to \Pphi \Pmu \Pmu$}
+{~}
+ \begin{minipage}{\textwidth}
+ \begin{center}
+ \includegraphics[width=0.65\textwidth]{images/bs2phipi.png}\\
+ \end{center}
+
+\begin{itemize}
+\item Last years LHCb measurement. %\href{http://arxiv.org/abs/1506.08777}{{\color{blue}{JHEP09 (2015) 179}}}.
+\item Suppressed by $\frac{f_s}{f_d}$.
+\item Cleaner because of narrow $\Pphi$ resonance.
+\item $3.3~\sigma$ deviation in SM in the $1-6\GeV^2$ bin.
+\end{itemize}
+
+
+\end{minipage}
+\textref{JHEP09 (2015) 179}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{BF of $\PLambdab \to \PLambda \Pmu \Pmu$}
+{~}
+ \begin{minipage}{\textwidth}
+
+ \begin{center}
+ \only<1>{
+ \includegraphics[width=0.65\textwidth]{images/Lb_BR.png}
+}
+ \only<2>{
+ \includegraphics[width=0.45\textwidth]{images/Lblow.png}
+\includegraphics[width=0.45\textwidth]{images/Lbhigh.png}
+
+}
+
+
+ \end{center}
+
+
+\begin{itemize}
+\item Last years LHCb measurement.% [{\color{blue}JHEP 06 (2015) 115]}.
+\item In total $\sim 300$ candidates in data set.
+\item Decay not present in the low $q^2$.
+
+\end{itemize}
+
+
+
+\end{minipage}
+\textref{JHEP 06 (2015) 115}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\begin{frame}{Angular analysis of $\PLambdab \to \PLambda \Pmu \Pmu$}
+{~}
+ \begin{minipage}{\textwidth}
+
+\begin{itemize}
+\item For the bins in which we have $>3~\sigma$ significance the forward backward asymmetry for the hadronic and leptonic system.
+\end{itemize}
+\begin{center}
+\includegraphics[width=0.9\textwidth]{{images/AFB_Lb}.png}
+\end{center}
+\begin{itemize}
+\item $A_{FB}^H$ is in good agreement with SM.
+\item $A_{FB}^{\ell}$ always in above SM prediction.
+\end{itemize}
+
+
+\end{minipage}
+\textref{JHEP 06 (2015) 115}
+
+ \vspace*{2.1cm}
+\end{frame}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+% Lepton Universlaity tests
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}
+{~}
+ \begin{minipage}{\textwidth}
+
+\begin{center}
+\begin{Huge}
+Lepton Universality tests
+\end{Huge}
+\end{center}
+
+
+
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Lepton universality test}
+{~}
+ \begin{minipage}{\textwidth}
+\begin{columns}
+\column{3.0in}
+\begin{itemize}
+\item Does the NP couple equally to all flavours?
+\includegraphics[width=0.9\textwidth]{images/uni2.png}
+\item Challenging analysis due to bremsstrahlung.
+\item Migration of events modeled by MC.
+\item Correct for bremsstrahlung.
+\item Take double ratio with $\PBplus \to \PJpsi \PKplus$ to cancel systematics.
+\item In $3\invfb$, LHCb measures: $R_K=0.745^{+0.090}_{-0.074}(stat.)^{+0.036}_{-0.036}(syst.)$
+\item Consistent with SM at $2.6\sigma$.
+
+\end{itemize}
+\column{2.0in}
+\includegraphics[width=0.99\textwidth]{images/RK.png}\\
+\includegraphics[width=0.95\textwidth]{images/diagramsRK.png}
+
+\end{columns}
+
+
+
+\end{minipage}
+ \vspace*{2.1cm}
+\textref{Phys. Rev. Lett. 113, 151601 (2014)}
+
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{More Lepton universality tests}
+{~}
+ \begin{minipage}{\textwidth}
+
+\begin{itemize}
+\item There is one other LUV decay recently measured by LHCb.
+\item $R(\PDstar)=\dfrac{\mathcal{B}(\PB \to \PDstar \Ptau \Pnu)}{\mathcal{B}(\PB \to \PDstar \Pmu \Pnu)}$
+\item Clean SM prediction: $R(\PDstar)=0.252(3)$, PRD 85 094025 (2012)
+\item LHCb result: $R(\PDstar)= 0.336 \pm 0.027 \pm 0.030$, HFAG average: $R(\PDstar)=0.322 \pm 0.022$
+\item $4.0~\sigma$ discrepancy wrt. SM.
+\end{itemize}
+
+\begin{center}
+
+\includegraphics[width=0.52\textwidth]{images/RDstar.png}
+
+\end{center}
+ \end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Explanation of anomalies}
+{~}
+ \begin{minipage}{\textwidth}
+ \ARROW Thanks to S. Descotes-Genon, L.Hofer, J.Matias, J.Virto we have a global fit to the anomalies.\\
+ \begin{center}
+ \includegraphics[width=0.75\textwidth]{images/quim2.png}
+ \end{center}
+\ARROW The fit prefer a modification of $C_9$ Wilson coefficient with a value of $C_9^{NP}=-1$, with a significance over $4\sigma$.\\
+\ARROW Many theories link might accommodate the observed deviations.
+
+\textref{arXiv:1510.04239}
+ \end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Explanation of anomalies}
+{~}
+ \begin{minipage}{\textwidth}
+
+\begin{itemize}
+\item We are not there yet!
+\item There might be something not taken into account in the theory.
+\item Resonances ($\PJpsi$, $\Ppsi(2S)$) tails can mimic NP effects.
+\item There might be some non factorizable QCD corrections.\\
+'' However, the central value of this effect would have to be significantly larger than expected on the basis of existing estimates'' \texttt{D.Straub, 1503.06199}
+.
+\end{itemize}
+
+\includegraphics[width=0.9\textwidth]{images/charmloop.png}
+
+
+
+ \end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{}
+\begin{center}
+\begin{Huge}
+$(g-2)_{\mu}$
+\end{Huge}
+\end{center}
+
+\end{frame}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Muon anomalous magnetic moment $(g-2)_{\mu}$}
+{~}
+ \begin{minipage}{\textwidth}
+\ARROW Dirac equations predict a muon magnetic moment $\overrightarrow{M}=g_{\mu} \frac{e}{2m_{\mu}}\overrightarrow{S}$ with a gyromagnetic ratio $g_{\mu}=2$. Experimentally $g_{\mu}>2$.\\
+\ARROW This anomaly $a_{\mu}$ arises from calculable quantum fluctuations:
+\begin{center}
+\includegraphics[width=0.8\textwidth]{images/gm2.png}
+\end{center}
+\ARROW SM value $a_{\mu}^{\rm SM}=(116 591 803 \pm 49) \times 10^{-11}$ [PDG 2014]\\
+\ARROW Experiment: $a_{\mu}^{\rm E821}=(116 592 091 \pm 63) \times 10^{-11}$ [PDG 2014]\\
+\ARROW Difference: $a_{\mu}^{\rm E821} -a_{\mu}^{\rm SM} =(288 \pm 80)\times 10^{-11}$ $\Leftrightarrow$ $3.6~\sigma$!\\
+\ARROW Underestimated uncertainties? SUSY? NP?\\
+\ARROW Fermilabs E989 should futher reduce the experimental error to $\pm16 \times 10^{-11}$.
+
+ \end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+%%% CP violation
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{$\gamma$ angle}
+{~}
+\begin{footnotesize}
+
+ \begin{minipage}{\textwidth}
+\ARROW $\gamma = \arg \left(- \frac{V_{ud}V_{ub}^{\ast} }{ V_{cd}V_{cb}^{\ast} }\right) \approx \arg(- \frac{V_{ub}^{\ast}}{V_{cb}^{\ast}})$ is the last well known CKM angles.\\
+\ARROW Can be determined by:
+\begin{itemize}
+\item Tree level processes, nearly insensitive to NP. Act as reference. Negligible theoretical uncertainty, using $\PB \to \PD \PK$.
+\item Loop processes, sensitive to NP.
+\end{itemize}
+\ARROW Comparing the two can reveal NP!
+\begin{columns}
+
+\column{2.2in}
+\includegraphics[width=0.9\textwidth]{images/gamma.png}
+
+\column{2.8in}
+\ARROW The LHCb combinations leads to: $\gamma = 70.9^{+7.1}_{-8.5}$.\\
+\ARROW Improved by $2^{\deg}$ compared to our previous result!\\
+\ARROW Other B-factories have 2 times larger errors:
+\begin{itemize}
+\item BaBar: $\gamma=(70\pm 18)^{\deg}$
+\item Belle: $\gamma=(73^{+18}_{-15})^{\deg}$
+
+\end{itemize}
+
+\end{columns}
+
+
+ \end{minipage}
+ \end{footnotesize}
+
+
+ \vspace*{2.1cm}
+\end{frame}
+
+
+
+\begin{frame}{Mixing induced CPV in $\PBs$}
+{~}
+\begin{small}
+
+ \begin{minipage}{\textwidth}
+\ARROW Interference between $\PBs$ decaying to $\PJpsi \Pphi$ either directly or by oscillations gives rise to CP violation phase: $\phi_s^{\PJpsi \Pphi}$
+\begin{center}
+\includegraphics[width=0.85\textwidth]{images/phis.png}
+\end{center}
+\ARROW In the Sm $\phi_s \approx -2 \beta+s = -(0.0376^{+0.0007}_{-0.0008})~\rm rad$, where $\beta_s=\arg \left(- \frac{V_{ts}V_{tb}^{\ast}}{V_{cs} V_{cb}^{\ast}} \right)$\\
+\ARROW At the leading order the same phase is expected $\PBs \to \PDs \PDs$ and $\PB \to \PJpsi \Ppi \Ppi$.\\
+\ARROW NP can enter in the $\PBs$ mixing!\\
+\ARROW Measured by simultaneous fit to $\PBs$ and $\bar{\PBs}$ decay rates:
+\begin{center}
+\includegraphics[width=0.9\textwidth]{images/phis2.png}
+
+\end{center}
+
+ \end{minipage}
+ \end{small}
+
+
+ \vspace*{2.1cm}
+\end{frame}
+
+
+
+\begin{frame}{Mixing induced CPV in $\PBs$}
+{~}
+\begin{small}
+
+ \begin{minipage}{\textwidth}
+\ARROW Interference between $\PBs$ decaying to $\PJpsi \Pphi$ either directly or by oscillations gives rise to CP violation phase: $\phi_s^{\PJpsi \Pphi}$
+\begin{center}
+\includegraphics[width=0.85\textwidth]{images/phis.png}
+\end{center}
+\ARROW In the Sm $\phi_s \approx -2 \beta+s = -(0.0376^{+0.0007}_{-0.0008})~\rm rad$, where $\beta_s=\arg \left(- \frac{V_{ts}V_{tb}^{\ast}}{V_{cs} V_{cb}^{\ast}} \right)$\\
+\ARROW At the leading order the same phase is expected $\PBs \to \PDs \PDs$ and $\PB \to \PJpsi \Ppi \Ppi$.\\
+\ARROW NP can enter in the $\PBs$ mixing!\\
+\ARROW Measured by simultaneous fit to $\PBs$ and $\bar{\PBs}$ decay rates:
+\begin{center}
+\includegraphics[width=0.9\textwidth]{images/phis2.png}
+
+\end{center}
+
+ \end{minipage}
+ \end{small}
+
+
+ \vspace*{2.1cm}
+\end{frame}
+
+
+
+
+
+\backupbegin
+
+\begin{frame}\frametitle{Backup}
+
+
+\end{frame}
+
+
+
+
+
+
+\begin{frame}{Theory implications}
+{~}
+ \begin{minipage}{\textwidth}
+
+\includegraphics[height=0.9\textheight]{images/table.png}
+
+
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{If not NP?}
+{~}
+\begin{minipage}{\textwidth}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
+\begin{itemize}
+\item How about our clean $P_i$ observables?
+\item The QCD cancel as mentioned only at leading order.
+\item Comparison to normal observables with the optimised ones.
+\end{itemize}
+\includegraphics[width=0.9\textwidth]{images/C9_S_P.png}
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Transversity amplitudes }
+{~}
+\begin{minipage}{\textwidth}
+
+$\color{JungleGreen}{\Rrightarrow}$ One can link the angular observables to transversity amplitudes
+{\tiny{
+\eqa{
+J_{1s} & = & \frac{(2+\beta_\ell^2)}{4} \left[|\apeL|^2 + |\apaL|^2 +|\apeR|^2 + |\apaR|^2 \right]
+ + \frac{4 m_\ell^2}{q^2} \re\left(\apeL\apeR^* + \apaL\apaR^*\right)\,,\nn\\[1mm]
+%
+J_{1c} & = & |\azeL|^2 +|\azeR|^2 + \frac{4m_\ell^2}{q^2} \left[|A_t|^2 + 2\re(\azeL^{}\azeR^*) \right] + \beta_\ell^2\, |A_S|^2 \,,\nn\\[1mm]
+%
+J_{2s} & = & \frac{ \beta_\ell^2}{4}\left[ |\apeL|^2+ |\apaL|^2 + |\apeR|^2+ |\apaR|^2\right],
+\hspace{0.92cm} J_{2c} = - \beta_\ell^2\left[|\azeL|^2 + |\azeR|^2 \right]\,,\nn\\[1mm]
+%
+J_3 & = & \frac{1}{2}\beta_\ell^2\left[ |\apeL|^2 - |\apaL|^2 + |\apeR|^2 - |\apaR|^2\right],
+\qquad J_4 = \frac{1}{\sqrt{2}}\beta_\ell^2\left[\re (\azeL\apaL^* + \azeR\apaR^* )\right],\nn \\[1mm]
+%
+J_5 & = & \sqrt{2}\beta_\ell\,\Big[\re(\azeL\apeL^* - \azeR\apeR^* ) - \frac{m_\ell}{\sqrt{q^2}}\,
+\re(\apaL A_S^*+ \apaR^* A_S) \Big]\,,\nn\\[1mm]
+%
+J_{6s} & = & 2\beta_\ell\left[\re (\apaL\apeL^* - \apaR\apeR^*) \right]\,,
+\hspace{2.25cm} J_{6c} = 4\beta_\ell\, \frac{m_\ell}{\sqrt{q^2}}\, \re (\azeL A_S^*+ \azeR^* A_S)\,,\nn\\[1mm]
+%
+J_7 & = & \sqrt{2} \beta_\ell\, \Big[\im (\azeL\apaL^* - \azeR\apaR^* ) +
+\frac{m_\ell}{\sqrt{q^2}}\, \im (\apeL A_S^* - \apeR^* A_S)) \Big]\,,\nn\\[1mm]
+%
+J_8 & = & \frac{1}{\sqrt{2}}\beta_\ell^2\left[\im(\azeL\apeL^* + \azeR\apeR^*)\right]\,,
+%
+\hspace{1.9cm} J_9 = \beta_\ell^2\left[\im (\apaL^{*}\apeL + \apaR^{*}\apeR)\right] \,,
+\label{Js}\nonumber}
+}}
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Link to effective operators}
+{~}
+\begin{minipage}{\textwidth}
+$\color{JungleGreen}{\Rrightarrow}$ So here is where the magic happens. At leading order the amplitudes can be written as (soft form factors):
+{\tiny{
+\eqa{
+\apeLR &=&\sqrt{2} N m_B(1- \hat s)\bigg[ (\Ceff9 + \Cpeff9) \mp (\C{10} + \Cp{10})
++\frac{2\hat{m}_b}{\hat s} (\Ceff7 + \Cpeff7) \bigg]\xi_{\bot}(E_{K^*}) \nn \\[2mm]
+\apaLR &=& -\sqrt{2} N m_B (1-\hat s)\bigg[(\Ceff9 - \Cpeff9) \mp (\C{10} - \Cp{10})
++\frac{2\hat{m}_b}{\hat s}(\Ceff7 - \Cpeff7) \bigg] \xi_{\bot}(E_{K^*}) \nn \\[2mm]
+\azeLR &=& -\frac{N m_B (1-\hat s)^2}{2 \hat{m}_{K^*} \sqrt{\hat s}} \bigg[ (\Ceff9 - \Cpeff9) \mp (\C{10} - \Cp{10}) + 2\hat{m}_b (\Ceff7 - \Cpeff7) \bigg]\xi_{\|}(E_{K^*}),
+\label{LargeRecoilAs}\nonumber}
+}}
+where $\hat s = q^2 /m_B^2$, $\hat{m}_i = m_i/m_B$. The $\xi_{\|,\bot }$ are the form factors. \\
+\pause
+$\color{JungleGreen}{\Rrightarrow}$ Now we can construct observables that cancel the $\xi$ form factors at leading order:
+\eq{P_5^{\prime} = \dfrac{J_5+\bar{J}_5}{2\sqrt{-(J_2^c+\bar{J}_2^c)(J_2^s+\bar{J}_2^s)} }\nonumber
+}
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Mass modelling}
+{~}
+\begin{minipage}{\textwidth}
+\begin{small}
+
+\begin{columns}
+\column{0.1in}
+{~}
+\column{2.5in}
+\ARROW The signal is modelled by a sum of two Crystal-Ball functions with common mean.\\
+\ARROW The background is a single exponential.\\
+\ARROW The base parameters are obtained from the proxy channel: $\PBd \to \PJpsi (\mu\mu) \PKstar$.\\
+\ARROW All the parameters are fixed in the signal pdf.\\
+\ARROW Scaling factors for resolution are determined from MC.\\
+\ARROW In fitting the rare mode only the signal, background yield and the slope of the exponential is left floating.\\
+\ARROW We found $624\pm30$ candidates in the most interesting $\left[1.1,6.0\right]~\GeV^2/c^4$ region \\ and $2398 \pm 57$ in the full range $\left[ 1.1, 19.\right]~\GeV^2/c^4$.
+\column{2.5in}
+\begin{center}
+\includegraphics[angle=-90,width=0.9\textwidth]{images/msignal.pdf}\\
+
+\end{center}
+\ARROW The S-wave fraction is extracted using a \texttt{LASS} model.
+\end{columns}
+
+\end{small}
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\iffalse
+%%%%%%%%%%%%%%%
+\begin{frame}{Monte Carlo corrections}
+{~}
+ \begin{minipage}{\textwidth}
+\begin{footnotesize}
+\ARROW No Monte Carlo simulation is perfect! One needs to correct for remaining differences.\\
+\ARROW We reweighted our $\PBd \to \PKstar \mu \mu$ Monte Carlo accordingly to differences between the $\PBd \to \PKstar \PJpsi$ in data (Splot) and Monte Carlo.
+\only<1>{
+\begin{center}
+\includegraphics[angle=-90,width=0.38\textwidth]{images/pt.pdf}
+\includegraphics[angle=-90,width=0.38\textwidth]{images/vertex.pdf}\\
+\includegraphics[angle=-90,width=0.38\textwidth]{images/nTracks.pdf}
+\end{center}
+}
+\only<2>{
+\begin{center}
+\includegraphics[angle=-90,width=0.38\textwidth]{images/eta_logy.pdf}
+\includegraphics[angle=-90,width=0.38\textwidth]{images/B0_p.pdf} \\
+\includegraphics[angle=-90,width=0.38\textwidth]{{images/bdt_data_mc_nominalMkpi}.pdf}
+\end{center}
+}
+
+\end{footnotesize}
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
+\fi
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Detector acceptance}
+{~}
+ \begin{minipage}{\textwidth}
+\begin{footnotesize}
+
+\begin{columns}
+
+\column{0.6\textwidth}
+\begin{itemize}
+\item Detector distorts our angular distribution.
+\item We need to model this effect.
+\item 4D function is used:
+\begin{align*}
+\epsilon (\cos \thetal, \cos \thetak, \phi, q^2) = \\\sum_{ijkl} P_i(\cos \thetal) P_j(\cos \thetak ) P_k(\phi) P_l(q^2),
+\end{align*}
+where $P_i$ is the Legendre polynomial of order $i$.
+\item We use up to $4^{th}, 5^{th}, 6^{th}, 5^{th}$ order for the $\cos \thetal, \cos \thetak, \phi, q^2$.
+\item The coefficients were determined using Method of Moments, with a huge simulation sample.
+\item The simulation was done assuming a flat phase space and reweighing the $q^2$ distribution to make is flat.
+
+\end{itemize}
+%\includegraphics[width=0.75\textwidth]{images/q2PHSP.png}
+
+
+
+\column{0.4\textwidth}
+%\only<1>{
+%\includegraphics[width=0.99\textwidth]{images/q2PHSP.png}\\
+%\includegraphics[width=0.99\textwidth]{images/q2PHSPw.png}
+%}
+
+\only<1>{
+\includegraphics[width=0.99\textwidth]{images/det.png}
+}
+\end{columns}
+
+
+\end{footnotesize}
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Control channel}
+{~}
+ \begin{minipage}{\textwidth}
+\begin{footnotesize}
+\begin{itemize}
+\item We tested our unfolding procedure on $\PB \to \PJpsi \PKstar$.
+\item The result is in perfect agreement with other experiments and our different analysis of this decay.
+\end{itemize}
+\end{footnotesize}
+\begin{center}
+\includegraphics[angle=-90,width=0.4\textwidth]{images/mlogjpsi.pdf}
+\includegraphics[angle=-90,width=0.4\textwidth]{images/mkpijpsi.pdf}\\
+\includegraphics[width=0.99\textwidth]{images/angles3.png}
+\end{center}
+
+
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{The columns of New Physics}
+{~}
+ \begin{minipage}{\textwidth}
+ \begin{center}
+ \includegraphics[width=0.94\textwidth]{images/columns.png}
+
+ \end{center}
+
+
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{$\PBd \to \PKstar \Pmu \Pmu$ results}
+{~}
+\begin{footnotesize}
+
+ \begin{minipage}{\textwidth}
+\ARROW In the maximum likelihood fit one could weight the events accordingly to the $\dfrac{1}{\varepsilon(\cos \thetal, \cos \thetak, \phi, q^2)}$\\
+\ARROW Better alternative is to put the efficiency into the maximum likelihood fit itself:
+\begin{align*}
+\mathcal{L}=\prod_{i=1}^N \epsilon_i(\Omega_i, q_i^2) \mathcal{P}(\Omega_i, q_i^2) / \int \epsilon(\Omega, q^2) \mathcal{P}(\Omega, q^2) d\Omega dq^2
+\end{align*}
+\ARROW Only the relative weights matters!\\
+\ARROW The Procedure was commissioned with TOY MC study.\\
+\ARROW Use Feldmann-Cousins to determine the uncertainties. \\
+\ARROW Angular background component is modelled with $2^{\rm nd }$ order Chebyshev polynomials, which was tested on the side-bands.\\
+\ARROW S-wave component treated as nuisance parameter.\\
+\includegraphics[angle=-90,width=0.33\textwidth]{{images/FC_Afb3}.pdf}
+\includegraphics[angle=-90,width=0.33\textwidth]{{images/FC_P11}.pdf}
+\includegraphics[angle=-90,width=0.33\textwidth]{{images/FC_P57}.pdf}
+
+\end{minipage}
+
+\end{footnotesize}
+\textref{JHEP 02 (2016) 104}
+
+ \vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Maximum likelihood fit - Results}
+{~}
+ \begin{minipage}{\textwidth}
+\begin{center}
+\only<1>{
+\includegraphics[angle=-90,width=0.45\textwidth]{images/FLPad.pdf}
+\includegraphics[angle=-90,width=0.45\textwidth]{images/S3Pad.pdf}\\
+\includegraphics[angle=-90,width=0.45\textwidth]{images/S4Pad.pdf}
+\includegraphics[angle=-90,width=0.45\textwidth]{images/S5Pad.pdf}
+}
+\only<2>{
+\includegraphics[angle=-90,width=0.45\textwidth]{images/AFBPad.pdf}
+\includegraphics[angle=-90,width=0.45\textwidth]{images/S7Pad.pdf}\\
+\includegraphics[angle=-90,width=0.45\textwidth]{images/S8Pad.pdf}
+\includegraphics[angle=-90,width=0.45\textwidth]{images/S9Pad.pdf}
+}
+
+
+\end{center}
+ \ARROW SM: \href{http://arxiv.org/abs/1411.3161}{ {\color{blue}Eur.Phys.J. C75 (2015) no.8, 382 }}
+
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Method of moments}
+{~}
+\begin{footnotesize}
+ \begin{minipage}{\textwidth}
+\ARROW See {\color{blue}{\href{http://arxiv.org/abs/1503.04100}{Phys.Rev.D91(2015)114012}}}, F.Beaujean , M.Chrzaszcz, N.Serra, D. van Dyk for details.\\
+\ARROW The idea behind Method of Moments is simple: Use orthogonality of spherical harmonics, $f_j(\overrightarrow{\Omega})$ to solve for coefficients within a $q^2$ bin:
+\begin{align*}
+\int f_i(\overrightarrow{\Omega}) f_j(\overrightarrow{\Omega}) = \delta_{ij}
+\end{align*}
+\begin{align*}
+M_i = \int \left( \dfrac{1}{d(\Gamma+ \bar{\Gamma})/dq^2} \right) \dfrac{d^3(\Gamma+\bar{\Gamma})}{d \overrightarrow{\Omega}} f_i(\overrightarrow{\Omega})d \Omega
+\end{align*}
+\ARROW Don’t have true angular distribution but we ''sample'' it with our data.\\
+\ARROW Therefore: $\int \to \sum$ and $M_i \to \widehat{M}_i$
+\begin{align*}
+\hat{M}_i=\dfrac{1}{\sum_e \omega_e} \sum_e \omega_e f_i(\overrightarrow{\Omega}_e)
+\end{align*}
+\ARROW The weight $\omega$ accounts for the efficiency. Again the normalization of weights does not matter.
+
+
+\end{minipage}
+\end{footnotesize}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+\begin{frame}{Amplitudes method}
+{~}
+\begin{footnotesize}
+ \begin{minipage}{\textwidth}
+
+\ARROW Fit for amplitudes as (continuous) functions of $q^2$ in the region: $q^2 \in \left[ 1.1. 6.0 \right]~\GeV^2/c^4$.\\
+\ARROW Needs some Ansatz:
+\begin{align*}
+A(q^2) = \alpha + \beta q^2+ \dfrac{\gamma}{q^2}
+\end{align*}
+\ARROW The assumption is tested extensively with toys.\\
+\ARROW Set of 3 complex parameters $ \alpha, \beta, \gamma $ per vector amplitude:\begin{itemize}
+\item {\color{Magenta}{$L, ~R$}}, {\color{Cerulean}{$0 ,~\| ,~\bot$}}, {\color{PineGreen}{$\Re ,~\Im$}} $\rightarrowtail$~~ $3 \times {\color{PineGreen}{2}} \times {\color{Cerulean}{3}} \times {\color{Magenta}{2}} = 36$ DoF.
+\item Scalar amplitudes: $+4$ DoF.
+\item Symmetries of the amplitudes reduces the total budget to: $28$.
+\end{itemize}
+\ARROW The technique is described in \href{http://arxiv.org/pdf/1504.00574v2.pdf}{\color{blue}{JHEP06(2015)084}}, U. Egede, M. Patel, K.A. Petridis.\\
+\ARROW Allows to build the observables as continuous functions of $q^2$:
+\begin{itemize}
+\item At current point the method is limited by statistics.
+\item In the future the power of this method will increase.
+\end{itemize}
+\ARROW Allows to measure the zero-crossing points for free and with smaller errors than previous methods.
+\end{minipage}
+\end{footnotesize}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+
+\begin{frame}{Amplitudes - results}
+{~}
+\begin{footnotesize}
+ \begin{minipage}{\textwidth}
+\begin{center}
+\begin{columns}
+\column{0.45\textwidth}
+\includegraphics[angle=-90,width=0.95\textwidth]{{images/amplitudes_AFBOverlay}.pdf}\\
+\includegraphics[angle=-90,width=0.95\textwidth]{{images/amplitudes_S4Overlay}.pdf}
+
+\column{0.45\textwidth}
+\includegraphics[angle=-90,width=0.95\textwidth]{{images/amplitudes_S5Overlay}.pdf}\\
+{~}\\{~}\\{~}\\{~}\\
+\begin{large}
+Zero crossing points:
+\end{large}
+\begin{align*}
+q_0(S_4) & <2.65 & {\rm{~at~}} & 95\% ~CL \\
+q_0(S_5) & \in \left[ 2.49,3.95 \right] & {\rm{~at~}} & 68\% ~CL \\
+q_0(A_{FB}) & \in \left[ 3.40, 4.87 \right] & {\rm{~at~}} & 68\% ~CL
+\end{align*}
+
+
+\end{columns}
+\end{center}
+
+\end{minipage}
+\end{footnotesize}
+ \vspace*{2.1cm}
+\end{frame}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+% Lepton non universality
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
+
+
+
+
+
+\backupend
+\end{document}
diff --git a/SM@LHC/mchrzasz.tex~ b/SM@LHC/mchrzasz.tex~
new file mode 100644
index 0000000..55f44a1
--- /dev/null
+++ b/SM@LHC/mchrzasz.tex~
@@ -0,0 +1,1284 @@
+\documentclass[11 pt,xcolor={dvipsnames,svgnames,x11names,table}]{beamer}
+
+\usepackage[english]{babel}
+\usepackage{polski}
+
+
+\usetheme[
+ bullet=circle, % Other option: square
+ bigpagenumber, % circled page number on lower right
+ topline=true, % colored bar at the top of the frame
+ shadow=false, % Shading for beamer blocks
+ watermark=BG_lower, % png file for the watermark
+ ]{Flip}
+
+%\logo{\kern+1.em\includegraphics[height=1cm]{SHiP-3_LightCharcoal}}
+
+
+\usepackage[lf]{berenis}
+\usepackage[LY1]{fontenc}
+\usepackage[utf8]{inputenc}
+
+\usepackage{emerald}
+\usefonttheme{professionalfonts}
+\usepackage[no-math]{fontspec}
+\defaultfontfeatures{Mapping=tex-text} % This seems to be important for mapping glyphs properly
+
+\setmainfont{Gillius ADF} % Beamer ignores "main font" in favor of sans font
+\setsansfont{Gillius ADF} % This is the font that beamer will use by default
+% \setmainfont{Gill Sans Light} % Prettier, but harder to read
+
+\setbeamerfont{title}{family=\fontspec{Gillius ADF}}
+
+\input t1augie.fd
+
+%\newcommand{\handwriting}{\fontspec{augie}} % From Emerald City, free font
+%\newcommand{\handwriting}{\usefont{T1}{fau}{m}{n}} % From Emerald City, free font
+% \newcommand{\handwriting}{} % If you prefer no special handwriting font or don't have augie
+
+%% Gill Sans doesn't look very nice when boldfaced
+%% This is a hack to use Helvetica instead
+%% Usage: \textbf{\forbold some stuff}
+%\newcommand{\forbold}{\fontspec{Arial}}
+
+\usepackage{graphicx}
+\usepackage[export]{adjustbox}
+
+\usepackage{amsmath}
+\usepackage{amsfonts}
+\usepackage{amssymb}
+\usepackage{bm}
+\usepackage{colortbl}
+\usepackage{mathrsfs} % For Weinberg-esque letters
+\usepackage{cancel} % For "SUSY-breaking" symbol
+\usepackage{slashed} % for slashed characters in math mode
+\usepackage{bbm} % for \mathbbm{1} (unit matrix)
+\usepackage{amsthm} % For theorem environment
+\usepackage{multirow} % For multi row cells in table
+\usepackage{arydshln} % For dashed lines in arrays and tables
+\usepackage{siunitx}
+\usepackage{xhfill}
+\usepackage{grffile}
+\usepackage{textpos}
+\usepackage{subfigure}
+\usepackage{tikz}
+
+%\usepackage{hepparticles}
+\usepackage[italic]{hepparticles}
+
+\usepackage{hepnicenames}
+
+% Drawing a line
+\tikzstyle{lw} = [line width=20pt]
+\newcommand{\topline}{%
+ \tikz[remember picture,overlay] {%
+ \draw[crimsonred] ([yshift=-23.5pt]current page.north west)
+ -- ([yshift=-23.5pt,xshift=\paperwidth]current page.north west);}}
+
+
+
+% % % % % % % % % % % % % % % % % % % % % % % % % % % % % % % % % % %
+\usepackage{tikzfeynman} % For Feynman diagrams
+\usetikzlibrary{arrows,shapes}
+\usetikzlibrary{trees}
+\usetikzlibrary{matrix,arrows} % For commutative diagram
+% http://www.felixl.de/commu.pdf
+\usetikzlibrary{positioning} % For "above of=" commands
+\usetikzlibrary{calc,through} % For coordinates
+\usetikzlibrary{decorations.pathreplacing} % For curly braces
+% http://www.math.ucla.edu/~getreuer/tikz.html
+\usepackage{pgffor} % For repeating patterns
+
+\usetikzlibrary{decorations.pathmorphing} % For Feynman Diagrams
+\usetikzlibrary{decorations.markings}
+\tikzset{
+ % >=stealth', %% Uncomment for more conventional arrows
+ vector/.style={decorate, decoration={snake}, draw},
+ provector/.style={decorate, decoration={snake,amplitude=2.5pt}, draw},
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+ fermion/.style={draw=gray, postaction={decorate},
+ decoration={markings,mark=at position .55 with {\arrow[draw=gray]{>}}}},
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+ scalarnoarrow/.style={dashed,draw=black},
+ electron/.style={draw=black, postaction={decorate},
+ decoration={markings,mark=at position .55 with {\arrow[draw=black]{>}}}},
+ bigvector/.style={decorate, decoration={snake,amplitude=4pt}, draw},
+}
+
+% TIKZ - for block diagrams,
+% from http://www.texample.net/tikz/examples/control-system-principles/
+% \usetikzlibrary{shapes,arrows}
+\tikzstyle{block} = [draw, rectangle,
+minimum height=3em, minimum width=6em]
+
+
+
+
+\usetikzlibrary{backgrounds}
+\usetikzlibrary{mindmap,trees} % For mind map
+\newcommand{\degree}{\ensuremath{^\circ}}
+\newcommand{\E}{\mathrm{E}}
+\newcommand{\Var}{\mathrm{Var}}
+\newcommand{\Cov}{\mathrm{Cov}}
+\newcommand\Ts{\rule{0pt}{2.6ex}} % Top strut
+\newcommand\Bs{\rule[-1.2ex]{0pt}{0pt}} % Bottom strut
+
+\graphicspath{{images/}} % Put all images in this directory. Avoids clutter.
+
+% SOME COMMANDS THAT I FIND HANDY
+% \renewcommand{\tilde}{\widetilde} % dinky tildes look silly, dosn't work with fontspec
+\newcommand{\comment}[1]{\textcolor{comment}{\footnotesize{#1}\normalsize}} % comment mild
+\newcommand{\Comment}[1]{\textcolor{Comment}{\footnotesize{#1}\normalsize}} % comment bold
+\newcommand{\COMMENT}[1]{\textcolor{COMMENT}{\footnotesize{#1}\normalsize}} % comment crazy bold
+\newcommand{\Alert}[1]{\textcolor{Alert}{#1}} % louder alert
+\newcommand{\ALERT}[1]{\textcolor{ALERT}{#1}} % loudest alert
+%% "\alert" is already a beamer pre-defined
+\newcommand*{\Scale}[2][4]{\scalebox{#1}{$#2$}}%
+
+\def\Put(#1,#2)#3{\leavevmode\makebox(0,0){\put(#1,#2){#3}}}
+
+\usepackage{gmp}
+\usepackage[final]{feynmp-auto}
+
+\usepackage[backend=bibtex,style=numeric-comp,firstinits=true]{biblatex}
+\bibliography{bib}
+\setbeamertemplate{bibliography item}[text]
+
+\makeatletter\let\frametextheight\beamer@frametextheight\makeatother
+
+% suppress frame numbering for backup slides
+% you always need the appendix for this!
+\newcommand{\backupbegin}{
+ \newcounter{framenumberappendix}
+ \setcounter{framenumberappendix}{\value{framenumber}}
+}
+\newcommand{\backupend}{
+ \addtocounter{framenumberappendix}{-\value{framenumber}}
+ \addtocounter{framenumber}{\value{framenumberappendix}}
+}
+
+
+\definecolor{links}{HTML}{2A1B81}
+%\hypersetup{colorlinks,linkcolor=,urlcolor=links}
+
+% For shapo's formulas:
+\def\lsi{\raise0.3ex\hbox{$<$\kern-0.75em\raise-1.1ex\hbox{$\sim$}}}
+\def\gsi{\raise0.3ex\hbox{$>$\kern-0.75em\raise-1.1ex\hbox{$\sim$}}}
+\newcommand{\lsim}{\mathop{\lsi}}
+\newcommand{\gsim}{\mathop{\gsi}}
+\newcommand{\wt}{\widetilde}
+%\newcommand{\ol}{\overline}
+\newcommand{\Tr}{\rm{Tr}}
+\newcommand{\tr}{\rm{tr}}
+\newcommand{\eqn}[1]{&\hspace{-0.7em}#1\hspace{-0.7em}&}
+\newcommand{\vev}[1]{\rm{$\langle #1 \rangle$}}
+\newcommand{\abs}[1]{\rm{$\left| #1 \right|$}}
+\newcommand{\eV}{\rm{eV}}
+\newcommand{\keV}{\rm{keV}}
+\newcommand{\GeV}{\rm{GeV}}
+\newcommand{\MeV}{\rm{MeV}}
+\newcommand{\im}{\rm{Im}}
+\newcommand{\re}{{\rm Re}}
+\newcommand{\invfb}{\rm{fb^{-1}}}
+\newcommand{\fixme}{\rm{{\color{red}{FIXME!}}}}
+\newcommand{\thetal}{\theta_l}
+\newcommand{\thetak}{\theta_k}
+\newcommand{\nn}{\nonumber}
+\newcommand{\eq}[1]{\begin{equation} #1 \end{equation}}
+%\newcommand{\eqn}[1]{\begin{displaymath} #1 \end{displaymath}}
+\newcommand{\eqa}[1]{\begin{eqnarray} #1 \end{eqnarray}}
+\newcommand{\apeL}{{A_\perp^L}}
+\newcommand{\apeR}{{A_\perp^R}}
+\newcommand{\apeLR}{{A_\perp^{L,R}}}
+\newcommand{\apaL}{{A_\|^L}}
+\newcommand{\apaR}{{A_\|^R}}
+\newcommand{\apaLR}{{A_\|^{L,R}}}
+\newcommand{\azeL}{{A_0^L}}
+\newcommand{\azeR}{{A_0^R}}
+\newcommand{\azeLR}{{A_0^{L,R}}}
+\newcommand{\Real}{\ensuremath{\mathcal{R}e}\xspace}
+\newcommand{\Imag}{\ensuremath{\mathcal{I}m}\xspace}
+
+\renewcommand{\C}[1]{{\cal C}_{#1}}
+\newcommand{\Ceff}[1]{{\cal C}^{\rm eff}_{#1}}
+\newcommand{\Cpeff}[1]{{\cal C}^{\rm eff\prime}_{#1}}
+\newcommand{\Cp}[1]{{\cal C}^{\prime}_{#1}}
+\def\FL {\ensuremath{F_{\mathrm{L}}}\xspace}
+\def\ATDPH {\ensuremath{A_{\mathrm{T,PR}}^{(2)}}\xspace}
+\def\ATImPH {\ensuremath{A_{\mathrm{T,PR}}^{\mathrm{Im}}}\xspace}
+\def\ATRePH {\ensuremath{A_{\mathrm{T,PR}}^{\mathrm{Re}}}\xspace}
+\def\FLPH {\ensuremath{F_{\mathrm{L,PR}}}\xspace}
+\def\ATDKG {\ensuremath{A_{\mathrm{T,\Kstarz \gamma}}^{(2)}}\xspace}
+\def\ATImKG {\ensuremath{A_{\mathrm{T,\Kstarz \gamma}}^{\mathrm{Im}}}\xspace}
+\def\ATReKG {\ensuremath{A_{\mathrm{T,\Kstarz \gamma}}^{\mathrm{Re}}}\xspace}
+\def\FLKG {\ensuremath{F_{\mathrm{L,\Kstarz \gamma}}}\xspace}
+\def\ATD {\ensuremath{A_{\mathrm{T}}^{(2)}}\xspace}
+\def\ATIm {\ensuremath{A_{\mathrm{T}}^{\mathrm{Im}}}\xspace}
+\def\ATRe {\ensuremath{A_{\mathrm{T}}^{\mathrm{Re}}}\xspace}
+
+
+
+\newcommand{\disp}{\displaystyle}
+\def\be{\begin{equation}}
+\def\ee{\end{equation}}
+\def\ba{\begin{eqnarray}}
+\def\ea{\end{eqnarray}}
+\def\d{\partial}
+\def\l{\left(}
+\def\r{\right)}
+\def\la{\langle}
+\def\ra{\rangle}
+\def\e{{\rm e}}
+\def\Br{{\rm Br}}
+
+
+
+\author{ {\fontspec{Trebuchet MS}Marcin Chrz\k{a}szcz} (Universit\"{a}t Z\"{u}rich, IFJ PAN)}
+\institute{UZH, IFJ PAN}
+\title[Anomalies in Flavour physics]{Anomalies in Flavour physics}
+\date{25 September 2014}
+
+
+\begin{document}
+\tikzstyle{every picture}+=[remember picture]
+
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+{
+\setbeamertemplate{sidebar right}{\llap{\includegraphics[width=\paperwidth,height=\paperheight]{bubble2}}}
+\begin{frame}[c]%{\phantom{title page}}
+\begin{center}
+\begin{center}
+ \begin{columns}
+ \begin{column}{0.75\textwidth}
+ \flushright\fontspec{Trebuchet MS}\bfseries \LARGE {Anomalies in Flavour physics}
+ \end{column}
+ \begin{column}{0.02\textwidth}
+ {~}
+ \end{column}
+ \begin{column}{0.23\textwidth}
+ % \hspace*{-1.cm}
+ \vspace*{-3mm}
+ \includegraphics[width=0.6\textwidth]{lhcb-logo}
+ \end{column}
+
+ \end{columns}
+\end{center}
+ \quad
+ \vspace{3em}
+\begin{columns}
+\begin{column}{0.44\textwidth}
+\flushright \vspace{-1.8em} {\fontspec{Trebuchet MS} \Large Marcin ChrzÄ…szcz\\\vspace{-0.1em}\small \href{mailto:mchrzasz@cern.ch}{mchrzasz@cern.ch}}
+
+\end{column}
+\begin{column}{0.53\textwidth}
+\includegraphics[height=1.3cm]{uzh-transp}{~}{~}
+\includegraphics[height=1.1cm]{ifj.png}
+\end{column}
+\end{columns}
+
+\vspace{1em}
+ \footnotesize\textcolor{gray}{Universit\"{a}t Z\"{u}rich, \\ Institute of Nuclear Physics, Polish Academy of Science}\normalsize\\
+\vspace{0.5em}
+
+ \textcolor{normal text.fg!50!Comment}{$5^{th}$ KEK Flavour Factory Workshop \\October 26-27,\\ Tokyo 2015}
+\end{center}
+\end{frame}
+}
+
+
+
+
+\iffalse
+
+\begin{frame}{Outline}
+
+ \begin{minipage}{\textwidth}
+
+\begin{enumerate}
+\item Why flavour is important.
+\item $\Pbeauty \to \Pstrange \ell \ell$ theory in a nutshell.
+\item LHCb measurements of $\Pbeauty \to \Pstrange \ell \ell$.
+\item Global fit to $\Pbeauty \to \Pstrange \ell \ell$ measurements.
+\item Conclusions.
+\end{enumerate}
+
+
+\end{minipage}
+ \vspace*{2.cm}
+\end{frame}
+
+\fi
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}\frametitle{Why rare decays?}
+\begin{columns}
+\column{4in}
+\begin{itemize}
+\item In SM allows only the charged interactions to change flavour.
+\begin{itemize}
+\item Other interactions are flavour conserving.
+\end{itemize}
+\item One can escape this constrain and produce $\Pbottom \to \Pstrange$ and $\Pbottom \to \Pdown$ at loop level.
+\begin{itemize}
+\item This kind of processes are suppressed in SM $\to$~Rare decays.
+\item New Physics can enter in the loops.
+\end{itemize}
+\end{itemize}
+\begin{center}
+\includegraphics[scale=0.3]{images/lupa.png}
+\includegraphics[scale=0.3]{images/example.png}
+\end{center}
+\column{1.5in}
+\includegraphics[width=0.61\textwidth]{images/couplings.png}
+\end{columns}
+
+\end{frame}
+
+
+\begin{frame}\frametitle{Tools}
+\begin{itemize}
+\item \textbf{Operator Product Expansion and Effective Field Theory}
+\end{itemize}
+\begin{columns}
+\column{0.1in}{~}
+\column{3.2in}
+\begin{align*}
+H_{eff} = - \dfrac{4G_f}{\sqrt{2}} V V^{\prime \ast}\ \sum_i \left[\underbrace{C_i(\mu)O_i(\mu)}_\text{left-handed} +\underbrace{C'_i(\mu)O'_i(\mu)}_\text{right-handed}\right],
+\end{align*}
+
+\column{2in}
+\begin{tiny}
+\begin{description}
+ \item[i=1,2] Tree
+ \item[i=3-6,8] Gluon penguin
+ \item[i=7] Photon penguin
+ \item[i=9.10] EW penguin
+ \item[i=S] Scalar penguin
+ \item[i=P] Pseudoscalar penguin
+ \end{description}
+
+\end{tiny}
+\end{columns}
+where $C_i$ are the Wilson coefficients and $O_i$ are the corresponding effective operators.
+\begin{center}
+\includegraphics[width=0.85\textwidth,height=3cm]{images/all.png}
+
+\end{center}
+
+
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\begin{frame}
+\only<1>{\frametitle{LHCb detector - tracking}
+\begin{columns}
+\column{3in}
+\includegraphics[width=0.9\textwidth]{images/1050px-Lhcbview.jpg}
+
+\column{2in}
+\includegraphics[width=0.95\textwidth]{images/sketch.png}
+\end{columns}
+\begin{itemize}
+\item Excellent Impact Parameter (IP) resolution ($20~\rm \mu m$).\\
+$\Rightarrow$ Identify secondary vertices from heavy flavour decays
+\item Proper time resolution $\sim~40~\rm fs$.\\
+$\Rightarrow$ Good separation of primary and secondary vertices.
+\item Excellent momentum ($\delta p/p \sim 0.4 - 0.6\%$) and inv. mass resolution.\\
+$\Rightarrow$ Low combinatorial background.
+
+\end{itemize}
+
+
+}
+
+\only<2>{\frametitle{LHCb detector - particle identification}
+\begin{columns}
+\column{3in}
+\includegraphics[width=0.9\textwidth]{images/1050px-Lhcbview.jpg}
+
+\column{2in}
+\includegraphics[width=0.95\textwidth]{images/cher.png}
+\end{columns}
+\begin{itemize}
+\item Excellent Muon identification $\epsilon_{\mu \to \mu} \sim 97\%$, $\epsilon_{\pi \to \mu} \sim 1-3\%$
+\item Good $\PK-\Ppi$ separation via RICH detectors, $\epsilon_{\PK \to \PK} \sim 95\%$, $\epsilon_{\Ppi \to \PK} \sim 5\%$.\\
+$\Rightarrow$ Reject peaking backgrounds.
+\item High trigger efficiencies, low momentum thresholds.
+Muons: $p_T > 1.76 \GeV$ at L0, $p_T > 1.0 \GeV$ at HLT1,\\
+$B \to \PJpsi X $: Trigger $\sim 90\%$.
+
+\end{itemize}
+
+
+}
+
+
+\end{frame}
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Recent measurements}
+{~}
+\only<1>{
+
+ \begin{minipage}{\textwidth}
+
+
+\begin{columns}
+
+\column{0.5\textwidth}
+$\color{JungleGreen}{\Rrightarrow}$ {\color{WildStrawberry}{Branching fractions:}}
+\begin{description}
+\item [$\PB^{0,\pm} \to \PK^{0,\pm} \Pmuon \APmuon$] {~}{~}LHCb, Mar 14
+\item [$\PB^{0} \to \PKstar \Pmuon \APmuon$] {~}{~}CMS, Jul 15
+\item [$\PBs \to \Pphi \Pmuon \APmuon$] {~}{~}{~}LHCb, Jun 15
+\item [$\PB^{\pm} \to \Ppi^{\pm} \Pmuon \APmuon$] {~}LHCb, Sep 15
+\item [$\PLambdab \to \PLambda \Pmuon \APmuon$] {~}{~}{~}{~}LHCb, Mar 15
+\item [$\PB \to\Pmuon \APmuon$] {~}{~}{~}{~}{~}CMS+LHCb, Jun 15
+\end{description}
+
+$\color{JungleGreen}{\Rrightarrow}$ {\color{WildStrawberry}{CP asymmetry:}}
+\begin{description}
+\item [$\PB^{\pm} \to \Ppi^{\pm} \Pmuon \APmuon$] {~}{~}LHCb, Sep 15
+\end{description}
+
+$\color{JungleGreen}{\Rrightarrow}$ {\color{WildStrawberry}{Isospin asymmetry:}}
+\begin{description}
+\item [$\PB \to \PK \Pmuon \APmuon$] {~}{~}{~}{~}{~}LHCb, Mar 14
+\end{description}
+
+
+\column{0.5\textwidth}
+$\color{JungleGreen}{\Rrightarrow}$ {\color{WildStrawberry}{Lepton Universality:}}
+\begin{description}
+\item [$\PB^{\pm} \to \PK^{\pm} \Plepton \APlepton$] {~}{~}LHCb, Jun 14
+\end{description}
+
+
+$\color{JungleGreen}{\Rrightarrow}$ {\color{WildStrawberry}{Angular:}}
+\begin{description}
+\item [$\PB^{0} \to \PK^{\ast} \Plepton \APlepton$] {~}{~}{~}LHCb, Jan 15
+\item [$\PB^{\pm} \to \PK^{\ast,\pm} \Plepton \APlepton$] BaBar, Aug 15
+\item [$\PBs \to \Pphi \Plepton \APlepton$] {~}{~}{~}LHCb, Jun 15
+\item [$\PLambdab \to \PLambda \Pmuon \APmuon$] {~}{~}LHCb, Mar 15
+\end{description}
+
+
+
+
+
+\end{columns}
+
+\end{minipage}
+}
+\only<2>{
+
+ \begin{minipage}{\textwidth}
+
+
+\begin{columns}
+
+\column{0.5\textwidth}
+$\color{JungleGreen}{\Rrightarrow}$ {\color{WildStrawberry}{Branching fractions:}}
+\begin{description}
+\item [{\color{red}{$\PB^{0,\pm} \to \PK^{0,\pm} \Pmuon \APmuon$}}] {~}{~}{\color{red}{LHCb, Mar 14}}
+\item [$\PB^{0} \to \PKstar \Pmuon \APmuon$] {~}{~}CMS, Jul 15
+\item [{\color{red}{$\PBs \to \Pphi \Pmuon \APmuon$}}] {~}{~}{~}{\color{red}{LHCb, Jun 15}}
+\item [$\PB^{\pm} \to \Ppi^{\pm} \Pmuon \APmuon$] {~}LHCb, Sep 15
+\item [$\PLambdab \to \PLambda \Pmuon \APmuon$] {~}{~}{~}{~}LHCb, Mar 15
+\item [{\color{red}{$\PB \to\Pmuon \APmuon$}}] {~}{~}{~}{~}{~}{\color{red}{CMS+LHCb, Jun 15}}
+\end{description}
+
+$\color{JungleGreen}{\Rrightarrow}$ {\color{WildStrawberry}{CP asymmetry:}}
+\begin{description}
+\item [$\PB^{\pm} \to \Ppi^{\pm} \Pmuon \APmuon$] {~}{~}LHCb, Sep 15
+\end{description}
+
+$\color{JungleGreen}{\Rrightarrow}$ {\color{WildStrawberry}{Isospin asymmetry:}}
+\begin{description}
+\item [$\PB \to \PK \Pmuon \APmuon$] {~}{~}{~}{~}{~}LHCb, Mar 14
+\end{description}
+
+
+\column{0.5\textwidth}
+$\color{JungleGreen}{\Rrightarrow}$ {\color{WildStrawberry}{Lepton Universality:}}
+\begin{description}
+\item [{\color{red}{$\PB^{\pm} \to \PK^{\pm} \Plepton \APlepton$}}] {~}{~}{\color{red}{LHCb, Jun 14}}
+\end{description}
+
+
+$\color{JungleGreen}{\Rrightarrow}$ {\color{WildStrawberry}{Angular:}}
+\begin{description}
+\item [{\color{red}{$\PB^{0} \to \PK^{\ast} \Plepton \APlepton$}}] {~}{~}{~}LHCb, Jan 15
+\item [{\color{red}{$\PB^{\pm} \to \PK^{\ast,\pm} \Plepton \APlepton$}}] {\color{red}{BaBar, Aug 15}}
+\item [$\PBs \to \Pphi \Plepton \APlepton$] {~}{~}{~}LHCb, Jun 15
+\item [{\color{red}{$\PLambdab \to \PLambda \Pmuon \APmuon$}}] {~}{~}{\color{red}{LHCb, Mar 15}}
+\end{description}
+
+\begin{alertblock}{}
+$>2~\sigma$ deviations from SM
+
+\end{alertblock}
+
+\end{columns}
+
+\end{minipage}
+}
+
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{$\PBzero \to \PKstar \Pmuon \APmuon$ kinematics}
+{~}
+\begin{minipage}{\textwidth}
+
+$\color{JungleGreen}{\Rrightarrow}$ The kinematics of $\PBzero \to \PKstar \Pmuon \APmuon$ decay is described by three angles $\thetal$, $\thetak$, $\phi$ and invariant mass of the dimuon system ($q^2)$.
+
+ \only<1>{
+\begin{columns}
+\column{0.5\textwidth}
+
+$\color{JungleGreen}{\Rrightarrow}$ $\cos \thetak$: the angle between the direction of the kaon in the $\PKstar$ ($\overline{\PKstar}$) rest frame and the direction of the $\PKstar$ ($\overline{\PKstar}$) in the $\PBzero$ ($\APBzero$) rest frame.\\
+$\color{JungleGreen}{\Rrightarrow}$ $\cos \thetal$: the angle between the direction of the $\Pmuon$ ($\APmuon$) in the dimuon rest frame and the direction of the dimuon in the $\PBzero$ ($\APBzero$) rest frame.\\
+$\color{JungleGreen}{\Rrightarrow}$ $\phi$: the angle between the plane containing the $\Pmuon$ and $\APmuon$ and the plane containing the kaon and pion from the $\PKstar$.
+
+
+
+\column{0.5\textwidth}
+\includegraphics[width=0.95\textwidth]{images/angles.png}
+
+\end{columns}
+}
+ \only<2>{
+{\tiny{
+\eqa{\label{dist}
+\frac{d^4\Gamma}{dq^2\,d\!\cos\theta_K\,d\!\cos\theta_l\,d\phi}&=&\frac9{32\pi} \bigg[
+J_{1s} \sin^2\theta_K + J_{1c} \cos^2\theta_K + (J_{2s} \sin^2\theta_K + J_{2c} \cos^2\theta_K) \cos 2\theta_l\nn\\[1.5mm]
+&&\hspace{-2.7cm}+ J_3 \sin^2\theta_K \sin^2\theta_l \cos 2\phi + J_4 \sin 2\theta_K \sin 2\theta_l \cos\phi + J_5 \sin 2\theta_K \sin\theta_l \cos\phi \nn\\[1.5mm]
+&&\hspace{-2.7cm}+ (J_{6s} \sin^2\theta_K + {J_{6c} \cos^2\theta_K}) \cos\theta_l
++ J_7 \sin 2\theta_K \sin\theta_l \sin\phi + J_8 \sin 2\theta_K \sin 2\theta_l \sin\phi \nn\\[1.5mm]
+&&\hspace{-2.7cm}+ J_9 \sin^2\theta_K \sin^2\theta_l \sin 2\phi \bigg]\,,
+\nonumber}
+}}\\{~}\\
+$\color{JungleGreen}{\Rrightarrow}$ This is the most general expression of this kind of decay.\\
+$\color{JungleGreen}{\Rrightarrow}$ The $CP$ averaged angular observables are defined:\\
+\eq{
+S_i = \dfrac{J_i+ \bar{J}_i}{(d \Gamma + d \bar{\Gamma})/dq^2}\nonumber
+}
+
+}
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Transversity amplitudes }
+{~}
+\begin{minipage}{\textwidth}
+
+$\color{JungleGreen}{\Rrightarrow}$ One can link the angular observables to transversity amplitudes
+{\tiny{
+\eqa{
+J_{1s} & = & \frac{(2+\beta_\ell^2)}{4} \left[|\apeL|^2 + |\apaL|^2 +|\apeR|^2 + |\apaR|^2 \right]
+ + \frac{4 m_\ell^2}{q^2} \re\left(\apeL\apeR^* + \apaL\apaR^*\right)\,,\nn\\[1mm]
+%
+J_{1c} & = & |\azeL|^2 +|\azeR|^2 + \frac{4m_\ell^2}{q^2} \left[|A_t|^2 + 2\re(\azeL^{}\azeR^*) \right] + \beta_\ell^2\, |A_S|^2 \,,\nn\\[1mm]
+%
+J_{2s} & = & \frac{ \beta_\ell^2}{4}\left[ |\apeL|^2+ |\apaL|^2 + |\apeR|^2+ |\apaR|^2\right],
+\hspace{0.92cm} J_{2c} = - \beta_\ell^2\left[|\azeL|^2 + |\azeR|^2 \right]\,,\nn\\[1mm]
+%
+J_3 & = & \frac{1}{2}\beta_\ell^2\left[ |\apeL|^2 - |\apaL|^2 + |\apeR|^2 - |\apaR|^2\right],
+\qquad J_4 = \frac{1}{\sqrt{2}}\beta_\ell^2\left[\re (\azeL\apaL^* + \azeR\apaR^* )\right],\nn \\[1mm]
+%
+J_5 & = & \sqrt{2}\beta_\ell\,\Big[\re(\azeL\apeL^* - \azeR\apeR^* ) - \frac{m_\ell}{\sqrt{q^2}}\,
+\re(\apaL A_S^*+ \apaR^* A_S) \Big]\,,\nn\\[1mm]
+%
+J_{6s} & = & 2\beta_\ell\left[\re (\apaL\apeL^* - \apaR\apeR^*) \right]\,,
+\hspace{2.25cm} J_{6c} = 4\beta_\ell\, \frac{m_\ell}{\sqrt{q^2}}\, \re (\azeL A_S^*+ \azeR^* A_S)\,,\nn\\[1mm]
+%
+J_7 & = & \sqrt{2} \beta_\ell\, \Big[\im (\azeL\apaL^* - \azeR\apaR^* ) +
+\frac{m_\ell}{\sqrt{q^2}}\, \im (\apeL A_S^* - \apeR^* A_S)) \Big]\,,\nn\\[1mm]
+%
+J_8 & = & \frac{1}{\sqrt{2}}\beta_\ell^2\left[\im(\azeL\apeL^* + \azeR\apeR^*)\right]\,,
+%
+\hspace{1.9cm} J_9 = \beta_\ell^2\left[\im (\apaL^{*}\apeL + \apaR^{*}\apeR)\right] \,,
+\label{Js}\nonumber}
+}}
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Link to effective operators}
+{~}
+\begin{minipage}{\textwidth}
+$\color{JungleGreen}{\Rrightarrow}$ So here is where the magic happens. At leading order the amplitudes can be written as:
+{\tiny{
+\eqa{
+\apeLR &=&\sqrt{2} N m_B(1- \hat s)\bigg[ (\Ceff9 + \Cpeff9) \mp (\C{10} + \Cp{10})
++\frac{2\hat{m}_b}{\hat s} (\Ceff7 + \Cpeff7) \bigg]\xi_{\bot}(E_{K^*}) \nn \\[2mm]
+\apaLR &=& -\sqrt{2} N m_B (1-\hat s)\bigg[(\Ceff9 - \Cpeff9) \mp (\C{10} - \Cp{10})
++\frac{2\hat{m}_b}{\hat s}(\Ceff7 - \Cpeff7) \bigg] \xi_{\bot}(E_{K^*}) \nn \\[2mm]
+\azeLR &=& -\frac{N m_B (1-\hat s)^2}{2 \hat{m}_{K^*} \sqrt{\hat s}} \bigg[ (\Ceff9 - \Cpeff9) \mp (\C{10} - \Cp{10}) + 2\hat{m}_b (\Ceff7 - \Cpeff7) \bigg]\xi_{\|}(E_{K^*}),
+\label{LargeRecoilAs}\nonumber}
+}}
+where $\hat s = q^2 /m_B^2$, $\hat{m}_i = m_i/m_B$. The $\xi_{\|,\bot }$ are the form factors. \\
+\pause
+$\color{JungleGreen}{\Rrightarrow}$ Now we can construct observables that cancel the $\xi$ form factors at leading order:
+\eq{P_5^{\prime} = \dfrac{J_5+\bar{J}_5}{2\sqrt{-(J_2^c+\bar{J}_2^c)(J_2^s+\bar{J}_2^s)} }\nonumber
+}
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+% symmetries
+\begin{frame}{Symmetries in $\PB \to \PKstar \Pmu \Pmu$}
+{~}
+\begin{minipage}{\textwidth}
+$\color{JungleGreen}{\Rrightarrow}$ We have 12 angular coefficients ($S_i$).\\
+$\color{JungleGreen}{\Rrightarrow}$ There exists 4 symmetry transformations that leave the angular distributions non changed:
+\begin{tiny}
+\eq{
+n_\|=\binom{A_\|^L}{A_\|^{R*}}\ ,\quad
+n_\bot=\binom{A_\bot^L}{-A_\bot^{R*}}\ ,\quad
+n_0=\binom{A_0^L}{A_0^{R*}}\ .\nonumber
+}
+\end{tiny}
+\begin{tiny}
+\eq{
+ n_i^{'} = U n_i=
+ \left[
+ \begin{array}{ll}
+ e^{i\phi_L} & 0 \\
+ 0 & e^{-i \phi_R}
+ \end{array}
+ \right]
+ \left[
+ \begin{array}{rr}
+ \cos \theta & -\sin \theta \\
+ \sin \theta & \cos \theta
+ \end{array}
+ \right]
+ \left[
+ \begin{array}{rr}
+ \cosh i \tilde{\theta} & -\sinh i \tilde{\theta} \\
+ - \sinh i \tilde{\theta} & \cosh i \tilde{\theta}
+ \end{array}
+ \right]
+ n_i \,.
+ \label{symmassless}\nonumber}
+\end{tiny}
+$\color{JungleGreen}{\Rrightarrow}$ Using this symmetries one can show that there are 8 independent observables. The pdf can be wrote as:
+\begin{tiny}
+\begin{align*}
+\left.\frac{1}{{\rm d}(\Gamma+\bar{\Gamma})/{\rm d}q^2}\frac{{\rm d}(\Gamma+\bar{\Gamma})}{{\rm dcos}\thetal\,{\rm dcos}\thetak\,{\rm d}\phi}\right|_{\rm P} =
+\tfrac{9}{32\pi}\bigl[
+&\tfrac{3}{4} (1-{F_{\rm L}})\sin^2\thetak \label{eq:pdfpwave}\\[-0.75em]
+&+ {F_{\rm L}}\cos^2\thetak + \tfrac{1}{4}(1-{F_{\rm L}})\sin^2\thetak\cos 2\thetal\nonumber\\
+&- {F_{\rm L}} \cos^2\thetak\cos 2\thetal + {S_3}\sin^2\thetak \sin^2\thetal \cos 2\phi\nonumber\\
+&+ {S_4} \sin 2\thetak \sin 2\thetal \cos\phi + {S_5}\sin 2\thetak \sin \thetal \cos \phi\nonumber\\
+&+ \tfrac{4}{3} {A_{\rm FB}} \sin^2\thetak \cos\thetal + {S_7} \sin 2\thetak \sin\thetal \sin\phi\nonumber\\
+&+ {S_8} \sin 2\thetak \sin 2\thetal \sin\phi + {S_9}\sin^2\thetak \sin^2\thetal \sin 2\phi \nonumber
+\bigr].
+%\end{split}
+%\bigr],\
+\end{align*}
+\end{tiny}
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+
+
+
+
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{LHCb update of the $\PBzero \to \PKstar \Pmuon \APmuon$, Selection}
+{~}
+\begin{minipage}{\textwidth}
+\begin{columns}
+
+\column{0.5\textwidth}
+\begin{itemize}
+\item \href{https://lhcb.web.cern.ch/lhcb/Physics-Results/LHCb-CONF-2015-002.pdf}{{\color{blue}{LHCb-CONF-2015-002}}}
+\item PID, kinematics and isolation variables used in a Boosted Decision Tree (BDT) to reject background.
+\item Reject the regions of $\PJpsi$ and $\Ppsi(2S)$.
+\item Specific vetos for backgrounds: $\PLambdab \to \Pproton \PK \Pmu \Pmu$, $\PBs \to \Pphi \Pmu \Pmu$, etc.
+\item Using k-Fold technique and signal proxy $\PB \to \PJpsi \PKstar$ for training the BDT.
+\item Improved selection allowed for finer binning than the $1\invfb$ analysis.
+\end{itemize}
+
+
+\column{0.5\textwidth}
+
+\includegraphics[width=0.88\textwidth]{images/Fig1.pdf} \\
+\includegraphics[width=0.88\textwidth]{images/fold.png}
+
+\end{columns}
+
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{LHCb update of the $\PBzero \to \PKstar \Pmuon \APmuon$, Selection}
+{~}
+\begin{minipage}{\textwidth}
+
+\begin{itemize}
+\item Signal modelled by a sum of two Crystal-Ball functions.
+\item Shape is defined using $\PB \to \PJpsi \PKstar$ and corrected for $q^2$ dependency.
+\item Combinatorial background modelled by exponent.
+\end{itemize}
+
+\begin{columns}
+\column{0.5\textwidth}
+\begin{itemize}
+\item $\PK \Ppi$ system:
+\begin{itemize}
+\item Rel. Breit Wigner for P-wave
+\item Lass model for the S-wave.
+\item Linear model for background.
+\item Reduced the systematic compared to previous analysis.
+\end{itemize}
+\end{itemize}
+
+\column{0.5\textwidth}
+
+\includegraphics[width=0.88\textwidth]{images/pbkg}
+
+\end{columns}
+
+\begin{large}
+\begin{itemize}
+\item In total we found $2398\pm57$ candidates in the $(0.1,19)~\GeV^2$ $q^2$ region.
+\item $624 \pm 30$ candidates in the theoretically the most interesting $(1.1-6.0)~\GeV^2$ region.
+\end{itemize}
+\end{large}
+
+
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Detector acceptance}
+{~}
+\begin{minipage}{\textwidth}
+\begin{columns}
+
+\column{0.6\textwidth}
+\begin{itemize}
+\item Detector distorts our angular distribution.
+\item We need to model this effect.
+\item 4D function is used:
+\begin{align*}
+\epsilon (\cos \thetal, \cos \thetak, \phi, q^2) = \\\sum_{ijkl} c_{ijkl} P_i(\cos \thetal) P_j(\cos \thetak ) P_k(\phi) P_l(q^2),
+\end{align*}
+where $P_i$ is the Legendre polynomial of order $i$.
+\item We use up to $4^{th}, 5^{th}, 6^{th}, 5^{th}$ order for the $\cos \thetal, \cos \thetak, \phi, q^2$.
+\end{itemize}
+
+
+
+
+\column{0.4\textwidth}
+\includegraphics[width=0.99\textwidth]{images/det.png}
+\end{columns}
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Control channel}
+{~}
+\begin{minipage}{\textwidth}
+
+
+\begin{itemize}
+\item We tested our unfolding procedure on $\PB \to \PJpsi \PKstar$.
+\item The result is in perfect agreement with other experiments and our different analysis of this decay.
+\end{itemize}
+
+\begin{columns}
+
+\column{0.5\textwidth}
+
+\includegraphics[width=0.95\textwidth]{images/mlogjpsi.png}
+\column{0.5\textwidth}
+\includegraphics[width=0.95\textwidth]{images/mkpijpsi.png}
+
+\end{columns}
+
+
+\includegraphics[width=0.99\textwidth]{images/angles2.png}
+
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%5
+\begin{frame}\frametitle{$\PBzero \rightarrow \PK^{\ast} \Pmu \Pmu$ results}
+ \begin{minipage}{\textwidth}
+\begin{columns}
+\column{2.5in}
+\includegraphics[angle=-90,width=0.95\textwidth]{images/Fig5a.pdf}\\
+\includegraphics[angle=-90,width=0.95\textwidth]{images/Fig5c.pdf}
+\column{2.5in}
+\includegraphics[angle=-90,width=0.95\textwidth]{images/Fig5b.pdf}\\
+\includegraphics[angle=-90,width=0.95\textwidth]{images/Fig5d.pdf}
+\end{columns}
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+ %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%5
+\begin{frame}\frametitle{$\PBzero \rightarrow \PK^{\ast} \Pmu \Pmu$ results}
+ \begin{minipage}{\textwidth}
+\begin{columns}
+\column{2.5in}
+\includegraphics[angle=-90,width=0.95\textwidth]{images/Fig5e.pdf}\\
+\includegraphics[angle=-90,width=0.95\textwidth]{images/Fig5f.pdf}
+\column{2.5in}
+\includegraphics[angle=-90,width=0.95\textwidth]{images/Fig5g.pdf}\\
+\includegraphics[angle=-90,width=0.95\textwidth]{images/Fig5h.pdf}
+\end{columns}
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Results in $\PB \to \PKstar \Pmu \Pmu$}
+ \begin{minipage}{\textwidth}
+ \begin{center}
+ \includegraphics[angle=-90,width=0.65\textwidth]{images/Fig17.pdf}\\
+ \end{center}
+
+\begin{itemize}
+\item Tension with $3~\invfb$ gets confirmed!
+\item The two bins deviate both in $2.8~\sigma$ from SM prediction.
+\item Result compatible with previous result.
+\end{itemize}
+
+
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Branching fraction measurements of $\PB \to \PKstar^{\pm} \Pmu \Pmu$}
+{~}
+\includegraphics[width=0.5\textwidth]{images/ksmumu_BF.png}
+\includegraphics[width=0.5\textwidth]{images/kmumu_BF.png}
+
+\begin{center}
+\begin{columns}
+
+\column{0.4\textwidth}
+\begin{itemize}
+\item Despite large theoretical errors the results are consistently smaller then SM prediction.
+\end{itemize}
+\column{0.6\textwidth}
+\includegraphics[width=0.87\textwidth]{images/bukst_BF.png}
+
+
+\end{columns}
+
+
+\end{center}
+\vspace*{2.1cm}
+\end{frame}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Branching fraction measurements of $\PBs \to \Pphi \Pmu \Pmu$}
+{~}
+\begin{minipage}{\textwidth}
+ \begin{center}
+ \includegraphics[height=4cm]{images/bs2phipi.png}
+ \includegraphics[height=4cm]{images/BsSel.png}
+ \end{center}
+
+\begin{itemize}
+\item Recent LHCb measurement, \href{https://cds.cern.ch/record/2029820/files/JHEP09-179.pdf}{{\color{blue}{JHEPP09 (2015) 179}}}.
+\item Suppressed by $\frac{f_s}{f_d}$.
+\item Cleaner because of narrow $\Pphi$ resonance.
+\item $3.3~\sigma$ deviation in SM in the $1-6\GeV^2$ bin.
+\item Angular part in agreement with SM ($S_5$ is not accessible).
+\end{itemize}
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Branching fraction measurements of $\PLambdab \to \PLambda \Pmu \Pmu$}
+{~}
+\begin{minipage}{\textwidth}
+
+ \begin{center}
+ \only<1>{
+ \includegraphics[width=0.65\textwidth]{images/Lb_BR.png}
+}
+ \only<2>{
+ \includegraphics[width=0.45\textwidth]{images/Lblow.png}
+\includegraphics[width=0.45\textwidth]{images/Lbhigh.png}
+
+}
+
+
+ \end{center}
+
+
+\begin{itemize}
+\item This years LHCb measurement \href{http://arxiv.org/abs/1503.07138}{{\color{blue}{JHEP 06 (2015) 115}}}.
+\item In total $\sim 300$ candidates in data set.
+\item Decay not present in the low $q^2$.
+
+\end{itemize}
+
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\begin{frame}{Angular analysis of $\PLambdab \to \PLambda \Pmu \Pmu$}
+{~}
+\begin{minipage}{\textwidth}
+
+\begin{itemize}
+\item For the bins in which we have $>3~\sigma$ significance the forward backward asymmetry for the hadronic and leptonic system.
+\end{itemize}
+\begin{center}
+\includegraphics[width=0.9\textwidth]{{images/AFB_Lb}.png}
+\end{center}
+\begin{itemize}
+\item $A_{FB}^H$ is in good agreement with SM.
+\item $A_{FB}^{\ell}$ always in above SM prediction.
+\end{itemize}
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Lepton universality test}
+{~}
+\begin{minipage}{\textwidth}
+\begin{columns}
+\column{3.0in}
+\begin{itemize}
+\item If $\PZprime$ is responsible for the $P'_5$ anomaly, does it couple equally to all flavours?
+\includegraphics[width=0.9\textwidth]{images/uni2.png}
+\item Challenging analysis due to bremsstrahlung.
+\item Migration of events modeled by MC.
+\item Correct for bremsstrahlung.
+\item Take double ratio with $\PBplus \to \PJpsi \PKplus$ to cancel systematics.
+\item In $3\invfb$, LHCb measures $R_K=0.745^{+0.090}_{-0.074}(stat.)^{+0.036}_{-0.036}(syst.)$
+\item Consistent with SM at $2.6\sigma$.
+
+\end{itemize}
+\column{2.0in}
+\includegraphics[width=0.99\textwidth]{images/RK.png}\\
+\begin{itemize}
+\item \href{http://arxiv.org/abs/1406.6482}{{\color{blue}{Phys. Rev. Lett. 113, 151601 (2014)}}}.
+\end{itemize}
+\end{columns}
+
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Angular analysis of $\PBzero \to \PKstar \Pe \Pe$}
+{~}
+\only<1>{
+ \begin{minipage}{\textwidth}
+ \begin{itemize}
+ \item With the full data set ($3\invfb$) we performed angular analysis in $0.0004 < q^2 <1~\GeV^2$, \href{http://arxiv.org/abs/1503.07138}{{\color{blue}{JHEP 04 (2015) 064}}}.
+ \item Electrons channels are extremely challenging experimentally:
+ \begin{itemize}
+ \item Bremsstrahlung.
+ \item Trigger efficiencies.
+ \end{itemize}
+ \item Determine the angular observables: $\FL$, $\ATD$, $\ATRe$, $\ATIm$:
+ \end{itemize}
+\begin{equation}
+ \label{eq:physPars}
+ \begin{split}
+ \FL &=\frac{|A_0|^2}{|A_0|^2+|A_{||}|^2 + |A_\perp|^2}\\
+ \ATD &= \frac{|A_\perp|^2-|A_{||}|^2}{|A_\perp|^2+|A_{||}|^2}\\
+ \ATRe &= \frac{2\Real(A_{||L}A^*_{\perp L} + A_{||R}A^*_{\perp R})}{|A_{||}|^2 + |A_\perp|^2}\\
+ \ATIm &= \frac{2\Imag(A_{||L}A^*_{\perp L} + A_{||R}A^*_{\perp R})}{|A_{||}|^2 + |A_\perp|^2},
+\end{split}
+\end{equation}
+
+\end{minipage}
+}
+\only<2>{
+\begin{center}
+\includegraphics[width=0.5\textwidth]{images/Kstee.png}\\
+\end{center}
+\begin{itemize}
+\item Results in full agreement with the SM.
+\item Similar strength on $C_7$ Wilson coefficient as from $\Pbeauty \to \Pstrange \Pphoton$ decays.
+\end{itemize}
+
+\begin{center}
+\includegraphics[width=0.9\textwidth]{images/Kstee2.png}
+\end{center}
+
+}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Theory implications}
+{~}
+\begin{minipage}{\textwidth}
+
+\begin{itemize}
+\item A preliminary fit prepared by \texttt{S. Descotes-Genon, L. Hofer, J. Matias, J. Virto}, presented in \href{http://arxiv.org/abs/1510.04239}{\color{blue}{arXiv::1510.04239}}
+\item Took into the fit:
+\begin{itemize}
+\item $\mathcal{B} ( \PB \to X_s \Pphoton) = (3.36 \pm 0.23) \times 10^{-4} $, Misiak et. al. 2015.
+\item $\mathcal{B} ( \PB \to\Pmu \Pmu)$, theory: Bobeth et al 2013, experiment: LHCb+CMS average (2015)
+\item $\mathcal{B} ( \PB \to X_s \Pmu \Pmu$), Huber et al 2015
+\item $\mathcal{B} ( \PB \to \PK \Pmu \Pmu$),Bouchard et al 2013, 2015
+\item $\PB_{(s)} \to \PKstar(\Pphi) \Pmu \Pmu$, Horgan et al 2013
+\item $\PB \to \PK \Pe \Pe$, $\PB \to \PKstar \Pe \Pe$ and $R_k$.
+\end{itemize}
+%\item Overall there is $>4~\sigma$ discrepancy wrt. SM.
+\end{itemize}
+
+
+
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Theory implications}
+{~}
+\begin{minipage}{\textwidth}
+
+\begin{itemize}
+\item A preliminary fit prepared by \texttt{S. Descotes-Genon, L. Hofer, J. Matias, J. Virto}, presented in \href{http://arxiv.org/abs/1510.04239}{\color{blue}{arXiv::1510.04239}}
+\item The data can be explained by modifying the $C_9$ Wilson coefficient.
+\item Overall there is around $>4.~\sigma$ discrepancy wrt. SM.
+\end{itemize}
+\includegraphics[width=0.9\textwidth]{images/C9.png}
+
+
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{If not NP?}
+{~}
+\begin{minipage}{\textwidth}
+\begin{itemize}
+\item We are not there yet!
+\item There might be something not taken into account in the theory.
+\item Resonances ($\PJpsi$, $\Ppsi(2S)$) tails can mimic NP effects.
+\item There might be some non factorizable QCD corrections.\\
+'' However, the central value of this effect would have to be significantly larger than expected on the basis of existing estimates'' \texttt{D.Straub}, \href{http://arxiv.org/abs/1503.06199}{ {\color{blue}{arXiv::1503.06199}}}
+.
+\end{itemize}
+\only<1>{
+\includegraphics[width=0.9\textwidth]{images/charmloop.png}
+}
+\only<2>{
+\begin{center}
+\includegraphics[width=0.6\textwidth]{images/charmloop2.png}
+\end{center}
+}
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{There is more!}
+{~}
+\begin{minipage}{\textwidth}
+
+\begin{itemize}
+\item There is one other LUV decay recently measured by LHCb.
+\item $R(\PDstar)=\dfrac{\mathcal{B}(\PB \to \PDstar \Ptau \Pnu)}{\mathcal{B}(\PB \to \PDstar \Pmu \Pnu)}$
+\item Clean SM prediction: $R(\PDstar)=0.252(3)$, PRD 85 094025 (2012)
+\item LHCb result: $R(\PDstar)= 0.336 \pm 0.027 \pm 0.030$, HFAG average: $R(\PDstar)=0.322 \pm 0.022$
+\item $3.9~\sigma$ discrepancy wrt. SM.
+\end{itemize}
+
+\begin{center}
+
+\includegraphics[width=0.52\textwidth]{images/RDstar.png}
+
+\end{center}
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{Conclusions}
+{~}
+\begin{minipage}{\textwidth}
+\begin{itemize}
+\item Clear tensions wrt. SM predictions!
+\item Measurements cluster in the same direction.
+\item We are not opening the champagne yet!
+\item Still need improvement both on theory and experimental side.
+\item Time will tell if this is QCD+fluctuations or new Physics:
+\end{itemize}
+\pause
+''... when you have eliminated all the\\
+Standard Model explanations, whatever remains,\\
+however improbable, must be New Physics.''\\
+prof. Joaquim Matias
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}
+{~}
+\begin{minipage}{\textwidth}
+\begin{center}
+\begin{LARGE}
+Thank you for the attention!
+\end{LARGE}
+\includegraphics[width=0.8\textwidth]{images/Joke.jpg}
+
+\end{center}
+
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+
+
+\backupbegin
+
+\begin{frame}\frametitle{Backup}
+\topline
+
+\end{frame}
+
+\backupend
+
+
+
+
+\begin{frame}{Theory implications}
+{~}
+ \begin{minipage}{\textwidth}
+
+\includegraphics[height=0.9\textheight]{images/table.png}
+
+
+\end{minipage}
+ \vspace*{2.1cm}
+\end{frame}
+
+
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+\begin{frame}{If not NP?}
+{~}
+\begin{minipage}{\textwidth}
+\begin{itemize}
+\item How about our clean $P_i$ observables?
+\item The QCD cancel as mentioned only at leading order.
+\item Comparison to normal observables with the optimised ones.
+\end{itemize}
+\includegraphics[width=0.9\textwidth]{images/C9_S_P.png}
+
+
+\end{minipage}
+\vspace*{2.1cm}
+\end{frame}
+
+\end{document}
diff --git a/SM@LHC/mchrzasz.toc b/SM@LHC/mchrzasz.toc
new file mode 100644
index 0000000..429917f
--- /dev/null
+++ b/SM@LHC/mchrzasz.toc
@@ -0,0 +1,5 @@
+\boolfalse {citerequest}\boolfalse {citetracker}\boolfalse {pagetracker}\boolfalse {backtracker}\relax
+\defcounter {refsection}{0}\relax
+\beamer@endinputifotherversion {3.24pt}
+\defcounter {refsection}{0}\relax
+\select@language {english}
diff --git a/SM@LHC/mchrzasz_v2.pdf b/SM@LHC/mchrzasz_v2.pdf
new file mode 100644
index 0000000..ea5f4da
--- /dev/null
+++ b/SM@LHC/mchrzasz_v2.pdf
Binary files differ
diff --git a/SM@LHC/tikzfeynman.sty b/SM@LHC/tikzfeynman.sty
new file mode 100755
index 0000000..521fc65
--- /dev/null
+++ b/SM@LHC/tikzfeynman.sty
@@ -0,0 +1,43 @@
+% Tikz Feynman Diagrams
+% by Flip Tanedo
+% 4 January 2011, work in progress
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+%%% TIKZ - for drawing Feynman diagrams %%%%
+%%% ... use with pdflatex %%%%
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+\usepackage{tikz}
+\usetikzlibrary{arrows,shapes}
+\usetikzlibrary{trees}
+\usetikzlibrary{matrix,arrows} % For commutative diagram
+ % http://www.felixl.de/commu.pdf
+\usetikzlibrary{positioning} % For "above of=" commands
+\usetikzlibrary{calc,through} % For coordinates
+\usetikzlibrary{decorations.pathreplacing} % For curly braces
+\usepackage[tikz]{bclogo} % For cute logo boxes
+\usepackage{pgffor} % For repeating patterns
+
+\usetikzlibrary{decorations.pathmorphing} % For Feynman Diagrams
+\usetikzlibrary{decorations.markings}
+\tikzset{
+ % >=stealth', %% Different kind of arrows
+ vector/.style={decorate, decoration={snake}, draw},
+ fermion/.style={postaction={decorate},
+ decoration={markings,mark=at position .55 with {\arrow{>}}}},
+ fermionbar/.style={draw, postaction={decorate},
+ decoration={markings,mark=at position .55 with {\arrow{<}}}},
+ fermionnoarrow/.style={},
+ gluon/.style={decorate,
+ decoration={coil,amplitude=4pt, segment length=5pt}},
+ scalar/.style={dashed, postaction={decorate},
+ decoration={markings,mark=at position .55 with {\arrow{>}}}},
+ scalarbar/.style={dashed, postaction={decorate},
+ decoration={markings,mark=at position .55 with {\arrow{<}}}},
+ scalarnoarrow/.style={dashed,draw},
+%
+%% Special vectors (when you need to fine-tune wiggles)
+ provector/.style={decorate, decoration={snake,amplitude=2.5pt}, draw},
+ antivector/.style={decorate, decoration={snake,amplitude=-2.5pt}, draw},
+}
+
diff --git a/b2sll_barcelona/mchrzasz.aux b/b2sll_barcelona/mchrzasz.aux
index be8de6c..3d48e9a 100644
--- a/b2sll_barcelona/mchrzasz.aux
+++ b/b2sll_barcelona/mchrzasz.aux
@@ -209,48 +209,45 @@
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diff --git a/b2sll_barcelona/mchrzasz.log b/b2sll_barcelona/mchrzasz.log
index 75e6299..454398c 100644
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diff --git a/b2sll_barcelona/mchrzasz.pdf b/b2sll_barcelona/mchrzasz.pdf
index 596cae5..9afeaa6 100644
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+++ b/b2sll_barcelona/mchrzasz.pdf
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index 812311c..cc7a3b9 100644
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diff --git a/b2sll_barcelona/mchrzasz.tex b/b2sll_barcelona/mchrzasz.tex
index 0f1108b..056a802 100644
--- a/b2sll_barcelona/mchrzasz.tex
+++ b/b2sll_barcelona/mchrzasz.tex
@@ -1293,37 +1293,32 @@
\end{frame}
-%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
-\begin{frame}{There is more!}
-{~}
- \begin{minipage}{\textwidth}
-
-\begin{itemize}
-\item There is one other LUV decay recently measured by LHCb.
-\item $R(\PDstar)=\dfrac{\mathcal{B}(\PB \to \PDstar \Ptau \Pnu)}{\mathcal{B}(\PB \to \PDstar \Pmu \Pnu)}$
-\item Clean SM prediction: $R(\PDstar)=0.252(3)$, PRD 85 094025 (2012)
-\item LHCb result: $R(\PDstar)= 0.336 \pm 0.027 \pm 0.030$, HFAG average: $R(\PDstar)=0.322 \pm 0.022$
-\item $3.9~\sigma$ discrepancy wrt. SM.
-\end{itemize}
-
-\begin{center}
-
-\includegraphics[width=0.52\textwidth]{images/RDstar.png}
-
-\end{center}
- \end{minipage}
- \vspace*{2.1cm}
-\end{frame}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{frame}{Steps in the near future}
{~}
- \begin{minipage}{\textwidth}
-
+ \begin{minipage}{\textwidth}
+\begin{itemize}
+\item We are not there yet!
+\item There might be something not taken into account in the theory.
+\item Resonances ($\PJpsi$, $\Ppsi(2S)$) tails can mimic NP effects.
+\item There might be some non factorizable QCD corrections.\\
+'' However, the central value of this effect would have to be significantly larger than expected on the basis of existing estimates'' \texttt{D.Straub, 1503.06199}
+.
+\end{itemize}
+\only<1>{
+\includegraphics[width=0.9\textwidth]{images/charmloop.png}
+}
+\only<2>{
+\begin{center}
+\includegraphics[width=0.6\textwidth]{images/charmloop2.png}
+\end{center}
+}
- \end{minipage}
+\end{minipage}
+
\vspace*{2.1cm}
\end{frame}