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\title{Переход к формализму ОТО}
% \subtitle{в нашей Вселенной}
\author{С.И.Блинников}
\email{sergei.blinnikov@itep.ru,  sblinnikov@gmail.com}
\institution{ИТЭФ, ГАИШ, НГУ}
\slideCaption{Novosibirsk - \texttt{Prosper}}

\begin{document}

\maketitle

\begin{slide}{ }
% \begin{center}

%
    \textit{S.I.Blinnikov${}^{1,2}$}
\pv{1}
    \begin{minipage}[c]{6cm}
{${}^1$\it ИТЭФ = ITEP = Institute for Theoretical and  Experimental Physics,
Moscow}%\pv{1}
    \end{minipage}
    \begin{minipage}[c]{4cm}
 \IG{width=.6\textwidth}{itepm.ps}%\pv{1}
    \end{minipage} \hfill    %\pv{1}
\vskip 0.3cm
    \begin{minipage}[c]{6cm}
{${}^2$\it  ГАИШ = SAI = Sternberg Astronomical \\Institute, Moscow}\pv{1}
    \end{minipage}
    \begin{minipage}[c]{4cm}
   \IG{width=.6\textwidth}{sai-main.ps}\pv{1}
    \end{minipage}\hfill %\pv{1}
%     \begin{minipage}[c]{6cm}
% {${}^3$\it MPA, Garching}\pv{1}
%     \end{minipage}
%     \begin{minipage}[c]{4cm}
%    \IG{width=.6\textwidth}{MPA.ps}\pv{1}
%     \end{minipage}\hfill \pv{1}

%\end{center}

  \centerline{НГУ 29 сентября 2012}

\end{slide}


\bes{Most Luminous SNe}
\vglue -0.3cm
    \CIG{width=0.85\textwidth}{sn2006gyf2.ps}
\ens

\bes{\normalsize SN~2006gy -- сверхмощная сверхновая}
\vglue -0.3cm
    \begin{minipage}[c]{2.9cm}
{\small
{Ofek et al. 2007, ApJL,  astro-ph/0612408)}\pv{1}

{Smith et al. 2007, Sep. 10 ApJ, astro-ph/0612617)}\pv{1}
}
    \end{minipage}
    \begin{minipage}[c]{7.9cm}
    \CIG{width=0.95\textwidth}{sn2006gyf1.ps}\pv{1}
    \end{minipage}\hfill %\pv{1}
\ens

% На всякий случай красивый мультик:
% http://www.youtube.com/watch?v=17jymDn0W6U

\bes[Blinds]{Тёмная энергия Dark Energy (DE)}
\huge
\centering

Что такое Тёмная энергия?

{\tiny \dgreen Ответ до сих пор не известен!}

\bigskip

Как её нашли?


\ens



\bes{Scale factor $\boldsymbol{\Omega=1$, $\Omega=2}$}
\vglue -0.2cm

\begin{center}

\IG{width=.95\textwidth}{Image80.ps}

\end{center}
\ens

\bes{Scale factor $\boldsymbol{ \Omega_{\Lambda}=0.9, \; \Omega_m=0.1}$}
\vglue -0.2cm

\begin{center}

\IG{width=.95\textwidth}{Image78.ps}

\end{center}

\ens

\bes{Deceleration or Acceleration}

We see that in case of the accelerating growth of the scale factor
the objects in the past are more distant for {\red the same time difference
$t_0-t$}. I.e. they would appear {\blue fainter} than in standard decelerating
scenario with attractive gravity and no antigravity which may be due
to the $\Lambda$-term or, say, to $P=w\rho$ with $w < 0$.

However, the plots like above are not good to extract Omegas, since
$a(t)$ and $t$ are not directly observable.

{\large \red
Observables are redshifts and distances (the latter depend on a definition)
}

\ens

\bes{Nick Suntzeff 1}

\IG{width=0.95\textwidth,angle=0}{suntzeff1}

\ens

\bes{Driving force for Acceleration?}

{\dred  В слабых полях и при малых скоростях уравнения ОТО сводятся к Ньютону.}


$M=4\pi\rho R^3/3$, and Newton's laws
give us the energy conservation:
{\dblue
$$
   {u^2 \over 2}  = {G_{\rm N}M \over R} -\mbox{const} \;,
$$
}
If $  \rho \propto {1 / a^3}  \propto {M / R^3}$,
i.e.  $M={\rm const}$, then
$\dot a = u$ goes down (e.g. ordinary matter or CDM), -- {\red decelerating}.

If $\rho$ has a slowly changing or a constant component ($M$ grows!),
then ${\dot a}$ grows,  -- {\red accelerating}.
E.g. for $\rho=\rho_\Lambda={\rm const}$:
$$
{{\dot a}/ a} \to {\rm const}.
$$

\ens

\bes{Vacuum energy}

{\dblue
Introducing energy
into the vacuum is equivalent to introducing a cosmological constant
$\Lambda$
into Einstein's equations.
The vacuum energy has the form of a perfect fluid with
$$ %\begin{equation*}
  {\cal E} =  {{c^4\Lambda}\over{8\pi G}}\ .
$$ %\end{equation*}
Но
$$
dE +P dV = d({\cal E} V) + P dV = 0, \quad \Rightarrow P dV = - {\cal E} dV .
$$
We immediately get $P=-{\cal E}$, and
the energy density is independent of $a$, which is what
we would expect for the energy density of the vacuum.
%Since the energy density in matter and radiation decreases as the universe
%expands, if there is a nonzero vacuum energy it tends to win out over
%the long term (as long as the universe doesn't start contracting).
%If this happens, we say that the universe becomes {\bf vacuum-dominated}.
}
\ens


\bes{Distance Ladder}
\vglue -1.3cm
% \begin{center}
% \hspace{-.5cm}\includegraphics[clip,width=1.05\textwidth]{Extragalactic_distance_ladder}
\hspace{-.25cm}\includegraphics[width=1.0\textwidth]{Extragalactic_Distance_Ladder1}
% \end{center}

\ens

\bes{SN~2006X in M100 in Virgo Cluster}
% \vglue -0.7cm

\CIG{width=0.7\textwidth}{sn2006XIaInM100.ps}
\ens

\bes{Distance Ladder}
\vglue -1.3cm
% \begin{center}
% \hspace{-.5cm}\includegraphics[clip,width=1.05\textwidth]{Extragalactic_distance_ladder}
\hspace{-.25cm}\includegraphics[width=1.0\textwidth]{Extragalactic_Distance_Ladder1}
% \end{center}

\ens



\bes{Distance Ladder Cone}
\vglue -.3cm
% \begin{center}
% \hspace{-0.25cm}
\includegraphics[width=0.92\textwidth]{ladder23.eps}
% \end{center}

\ens


\bes{Distance Ladder - 2}
\vglue -1.3cm
% \begin{center}
% \hspace{-.5cm}\includegraphics[clip,width=1.05\textwidth]{Extragalactic_distance_ladder}
\hspace{-.25cm}\includegraphics[width=1.0\textwidth]{Extragalactic_Distance_LadderSnII1}
% \end{center}

\ens

\bes{Distance Ladder - 3}
\vglue -1.3cm
% \begin{center}
% \hspace{-.5cm}\includegraphics[clip,width=1.05\textwidth]{Extragalactic_distance_ladder}
\hspace{-.25cm}\includegraphics[width=1.0\textwidth]{Extragalactic_Distance_LadderSnIIMarked1}
% \end{center}

\ens


\bes{Hubble diagram, Feb 2004}
% \vglue -0.7cm
\centerline{\dred \large for SN~Ia (A.Riess et al.)}

%\IG{bb=56 56 566 566}{ariess04fig4}
%\IG{bb= 0 56 570 466}{ariess04fig4.ps}
\CIG{width=0.65\textwidth}{ariess04fig4.ps}
\ens

%\bes{$\Omega$  from SN~Ia: Riess et al. Feb 2004}
%{\blue Cosmological parameters from SN~Ia: Riess et al. Feb 2004}

%\begin{center}
%\IG{width=0.55\textwidth,angle=0}{ariess04fig8.ps}
%\end{center}

%\ens


\bes{Hubble diagram {\red SNLS}}
% \vglue -0.7cm
\begin{minipage}[c]{5cm}
\begin{center}
\includegraphics[width=\textwidth]{hubbleCorr.eps}
\end{center}
\end{minipage}
\begin{minipage}[c]{5cm}
{\small
The bottom plot shows the residuals for $\mu_B$
when $d_{\rm ph}(z)$ is for the best fit flat $\Lambda$-cosmology ($\Omega_M = 0.26, \; \Omega_\Lambda=0.74$). Dashed line is for the flat zero $\Lambda$ model.
Adopted with corrections from (Astier et al., 2006).
}
\end{minipage} \hfill    %\pv{1}
\ens


\bes{$(\Omega_m,\Omega_\Lambda)$ cosmology,  {\red SNLS}}
% \vglue -0.7cm
\begin{minipage}[c]{5cm}
\begin{center}
\includegraphics[width=\textwidth]{omol_contours.eps}
\end{center}
\end{minipage}
\begin{minipage}[c]{5cm}
{\small  {\red 68.3\%, 95.5\% and 99.7\%} confidence levels for
 the {\red SNLS} Hubble diagram
(solid contours),
 the {\dgreen SDSS} baryon acoustic oscillations (Eisenstein et al. 2005,
dotted lines), and the joint confidence contours (dashed lines).
(Astier et al., 2006).
}
\end{minipage} \hfill    %\pv{1}
\ens

\bes{$(\Omega_m,w)$ cosmology}
% \vglue -0.7cm
\begin{minipage}[c]{5cm}
\begin{center}
\includegraphics[width=\textwidth]{omw_contours.eps}
\end{center}
\end{minipage}
\begin{minipage}[c]{5cm}
{\small Contours at  {\red 68.3\%, 95.5\% and 99.7\%} confidence levels
for the fit to  cosmology with equation of state  $P=w\mathcal{E}$ for flat 3D space, from the {\red SNLS} Hubble diagram
alone, from the {\dgreen SDSS} baryon acoustic oscillations alone (Eisenstein et al. 2005),
and the joint confidence contours.
From (Astier et al., 2006).
}
\end{minipage} \hfill    %\pv{1}
\ens

\bes{Nick Suntzeff 1}

\IG{width=0.95\textwidth,angle=0}{suntzeff1}

\ens

\bes{Hubble diagram {\red SNLS}}
% \vglue -0.7cm
\begin{minipage}[c]{5cm}
\begin{center}
\includegraphics[width=\textwidth]{hubbleCorr.eps}
\end{center}
\end{minipage}
\begin{minipage}[c]{5cm}
{\small
The bottom plot shows the residuals for $\mu_B$
when $d_{\rm ph}(z)$ is for the best fit flat $\Lambda$-cosmology ($\Omega_M = 0.26, \; \Omega_\Lambda=0.74$). Dashed line is for the flat zero $\Lambda$ model.
Adopted with corrections from (Astier et al., 2006).
}
\end{minipage} \hfill    %\pv{1}
\ens


\bes{\small D.Rubin, E.V.Linder, M.Kowalski et al. ApJ 2009}
\begin{center}%
\includegraphics[width=0.47\textwidth]{colorOm-w0_sysinterp2}
\includegraphics[width=0.48\textwidth]{colorOm-w0_sys+sys_curvinterp2}
\end{center}
{\tiny 68.3\%, 95.4\%, and 99.7\% conf. levels on a constant
EOS $w$ and  $\Omega_m$ for the individual and combined data
sets.  The left panel shows individual and combined probes in the flat
universe case; the right panel repeats the combined systematics contour,
and also compares to the statistical only contour, and to the systematics
contour when simultaneously fitting for spatial curvature.
}
\ens

\bes{Nick Suntzeff 2}

\IG{width=0.95\textwidth,angle=0}{suntzeff2}

\ens

\bes{Nick Suntzeff 3}

\IG{width=0.95\textwidth,angle=0}{suntzeff3}

\ens


\bes[Wipe]{Surface of Last  Scattering}

\CIG{width=0.9\textwidth}{LastScatSurf.ps}

\ens


% \bes{Structure formation simulations}
% \begin{center}
%   \fbox{\href{run:/home/seb/Pres/movies/S2_960x640.avi}{Movie}}
% \end{center}
% \ens
%
%
% \bes{Проект SDSS, более новый}
%
% \begin{center}%
% %  \fbox{\href{run:../../../c/pres/movies/vv1a_9-25.mpg}{\dblue movie -- click here}}
%  \fbox{\href{run:/home/seb/Pres/movies/sdss_DR4.mov}
%    {\dblue SDSS Data Release 4 movie -- click here}}
% \end{center}
% \ens


\bes[Blinds]{Dark Matter and Dark Energy pie}
% \vglue -.5cm
% \centering{\red DM pie}
\CIG{width=0.95\textwidth}{DMpie}
\ens


\end{document}

