\section{2011 Nobel Prize Winners in Physics}

"The Nobel Prize in Physics 2011 was divided, one half awarded to 
Saul Perlmutter, the other half jointly to Brian P. Schmidt and 
Adam G. Riess for the discovery of the accelerating expansion of 
the Universe through observations of distant supernovae." the
nobelprize.org wrote.
\footnote{http://www.nobelprize.org/nobelprizes/physics/laureates/2011/ }

Two research teams, Supernova Cosmology Project (SCP) lead by
Saul Perlmutter and High-z Supernova Search Team (HZT) headed by
Brian Schmidt,  
raced to map the Universe by locating the most distant supernovae. 
The two research teams found over 50 distant supernovae which  
were dimmer than expected - this was a sign that the 
expansion of the Universe was accelerating [1], [2].


Theoretically, this was not new idea since Albert Einstein
came out the idea of cosmological constant (often marked Lambda).
Einstein did that because he was guided by the paradigm of 
the day that the Universe was static. When he heard the 
Edwin Hubble discovery that the Universe was actually expanding
he declared that the inclusion of the cosmological constant 
was his "biggest blunder". 
Since there was no observation for cosmological constant
after that most scientists assumed that Lambda is zero.
A series of papers were published in Astrophysics and Space Science
in the early 90's years before the supernova publications
calculated $\Omega_{\Lambda}$ from observed data.


\section{Earlier Publications About Positive Cosmological Constant}
 

Pa\'al et al. [3] used the so called pencil beam survey
[4] to find out whether the regularity found in the
galaxy distribution is quasiperiodical or not. 
It was found that $q_0$ was preferably negative [3]. Therefore 
a nonzero Lambda term was needed.
The preferred value was $\Omega_{\Lambda}$ equal 2/3.
This is very close to the value that later was observed by
the Nobel Prize winners.



\begin{figure}
{\includegraphics[angle=0,width=12.4cm]{horvathistvan_fig1.ps}}
\caption{This figure was published in Holba et al. 
(1994) (figure 8. in that article). 
The red line represents the flat cosmological model.  }
\end{figure}



In the second paper [5] a two parameter fit was made. 
The positive cosmological constant (negative $q_0$) found to be
still needed. In the third paper [6] optical and radio quasars
were also used to find the preferred cosmological parameters.
Figure 8. in that paper [6] showed the results (see figure).
As it was written the contour meant 80\% confidence level.
The preferred region is similar that the supernovae 
analisys later suggested. 
For comparison please see this www page 
http://vizion.galileowebcast.hu/HOI/Comparation.jpg  
Therefore those earlier suggestions also support 
the Nobel Prize winning results.



\acknowledgments


The author thanks for his supervisors, B. Luk\'acs and G. Pa\'al, 
to being part of these researches. Unfortunately, G. Pa\'al
died in 1992. This was surely affected the fact 
that these results were almost unrecognized.


\bigskip



{\bf REFERENCES}



[1] Perlmutter, S. et al., 1999, \apj,
    517, 565

[2] Riess, A. G. 
    et al., 1998, \aj, 116, 1009

[3] Pa\'al, G., 
Horv\'ath, I., \& Luk\'acs, B. 1992, \apss, 191, 107

[4] Broadhurst, T. J. et al., 
1990, Nature,  343, 726

[5] Holba, A., Horv\'ath, I., 
Luk\'acs, B., \& Pa\'al, G. 1992, \apss, 198, 111

[6] Holba, A., Horv\'ath, I., 
Luk\'acs, B., \& Pa\'al, G. 1994, \apss, 222, 65


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