  We report the results of our investigation on the possible existence of
supernova remnants (SNRs) in the nearby galaxy, NGC 1569, using the CCD imaging
and spectroscopic observations from the RTT150 telescope of TUG-TUBITAK in
Antalya, Turkey for two different observing periods. Using [S\,{\sc
ii}]/H$\alpha$ $\geq$ 0.4 standard criteria, the identification of 13 new SNR
candidates for this galaxy is proposed for two different epochs. We found the
[S\,{\sc ii}]/H$\alpha$ ratios ranging from 0.46--0.84 and H$\alpha$
intensities ranging from (2.2--32) $\times$ 10$^{-15}$ erg cm$^{-2}$ s$^{-1}$.
[S\,{\sc ii}]$\lambda\lambda$6716/6731 average flux ratio is calculated from
the optical spectra for only one possible SNR candidate. By using this ratio
the electron density, $N_{\rm e}$, is estimated to be 121 $\pm$ 17 cm$^{-3}$
and by using the [O\,{\sc iii}]$\lambda$5007/H$\beta$ ratio of the same
spectrum, the shock wave velocity, $V_{\rm s}$, is estimated to be between 100
< Vs < 150 km s$^{-1}$. Using {\it Chandra} data, we find that out of 13 SNR
candidates only 10 of them have yielded a spectrum with good statistics,
confirming the existence of 10 SNR candidates with matched positions in X-ray
region as well. We measure the 0.5--2 keV band flux down to 0.58 $\times$
10$^{-15}$ erg cm$^{-2}$ s$^{-1}$ for 10 X-ray sources. Our spectral analysis
revealed that spectra of the SNR candidates are best modelled with the
Collisional Ionisation Equilibrium plasma with a temperature range of 0.84 keV
< \textit{kT$_{e}$} < 1.36 keV.
