  Extremely metal-poor galaxies (XMPGs) at relatively low redshift are
excellent laboratories for studying galaxy formation and evolution in the early
universe. Much effort has been spent on identifying them from large-scale
spectroscopic surveys or spectroscopic follow-up observations. Previous work
has identified a few hundred XMPGs. In this work, we obtain a large sample of
223 XMPGs at $z<1$ from the early data of the Dark Energy Spectroscopic
Instrument (DESI). The oxygen abundance is determined using the direct $T_{\rm
e}$ method based on the detection of the [O III]$\lambda$4363 line. The sample
includes 95 confirmed XMPGs based on the oxygen abundance uncertainty;
remaining 128 galaxies are regarded as XMPG candidates. These XMPGs are only
0.01% of the total DESI observed galaxies. Their coordinates and other
proprieties are provided in the paper. The most XMPG has an oxygen abundance of
$\sim 1/34 Z_{\odot}$, stellar mass of about $1.5\times10^7 M_{\odot}$ and star
formation rate of 0.22 $M_{\odot}$ yr$^{-1}$. The two most XMPGs present
distinct morphologies suggesting different formation mechanisms. The local
environmental investigation shows that XMPGs preferentially reside in
relatively low-density regions. Many of them fall below the stellar
mass-metallicity relations (MZRs) of normal star-forming galaxies. From a
comparison of the MZR with theoretical simulations, it appears that XMPGs are
good analogs to high-redshift star-forming galaxies. The nature of these XMPG
populations will be further investigated in detail with larger and more
complete samples from the on-going DESI survey.
