  We report the first result of the clustering analysis of Sloan Digital Sky
Survey (SDSS) quasars. We compute the two-point correlation function (2PCF) of
SDSS quasars in redshift space at $8h^{-1}{\rm Mpc} < s < 500h^{-1}{\rm Mpc}$,
with particular attention to its baryonic signature. Our sample consists of
19986 quasars extracted from the SDSS Data Release 4 (DR4). The redshift range
of the sample is $0.72 \le z \le 2.24$ (the mean redshift is $\bar z = 1.46$)
and the reddening-corrected $i$-band apparent magnitude range is $15.0 \le
m_{i,{\rm rc}} \le 19.1$. Due to the relatively low number density of the
quasar sample, the bump in the power spectrum due to the baryon density,
$\Omega_{\rm b}$, is not clearly visible. The effect of the baryon density is,
however, to distort the overall shape of the 2PCF.The degree of distortion
makes it an interesting alternate measure of the baryonic signature. Assuming a
scale-independent linear bias and the spatially flat universe, i.e.,
$\Omega_{\rm b} + \Omega_{\rm d} + \Omega_\Lambda =1$, where $\Omega_{\rm d}$
and $\Omega_\Lambda$ denote the density parameters of dark matter and the
cosmological constant, we combine the observed quasar 2PCF and the predicted
matter 2PCF to put constraints on $\Omega_{\rm b}$ and $\Omega_\Lambda$. Our
result is fitted as $0.80- 2.8\Omega_{\rm b} < \Omega_\Lambda < 0.90 -
1.4\Omega_{\rm b}$ at the 2$\sigma$ confidence level, which is consistent with
results from other cosmological observations such as WMAP. (abridged)
