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We present the morphology and stellar population of 27 extremely metal poorgalaxies (EMPGs) at $z\sim0$ with metallicities of 0.01--0.1 Z$_{\odot}$. Weconduct multi-component surface brightness (SB) profile fitting for the deepSubaru/HSC $i$-band images of the EMPGs with the {\sc Galfit} software,carefully removing the SB contributions of tails. We find that the EMPGs with amedian stellar mass of $\log(M_{*}/{\rm M}_{\odot})=6.0$ have a medianS{\'e}rsic index of $n=1.1$ and a median effective radius of $r_{\rm e}=200$pc, suggesting that typical EMPGs have very compact disk. We compare the EMPGswith $z\sim6$ galaxies and local galaxies on the size-mass ($r_{\rm e}$-$M_*$)diagram, and identify that the majority of the EMPGs have a $r_{\rm e}$-$M_*$relation similar to $z\sim0$ star-forming galaxies rather than $z\sim6$galaxies. Not every EMPG is a local analog of high-$z$ young galaxies in the$r_{\rm e}$-$M_*$ relation. A spectrum of one pair of EMPG and tail, so faravailable, indicates that the tail is dynamically related to the EMPG with amedian velocity difference of $\Delta V=101\pm32$ km s$^{-1}$. Thismoderately-large $\Delta V$ cannot be explained by the dynamics of the tail,but likely by the infall on the tail. For the first time, we may identify themetal-poor star-forming system just now infalling into the tail.

astrophysical journal/the astrophysical journal

EMPRESS. III. Morphology, Stellar Population, and Dynamics of Extremely  Metal Poor Galaxies (EMPGs): Are EMPGs Local Analogs of High-$z$ Young  Galaxies?