We examine whether the radial acceleration relation (RAR) of dwarf galaxies can be explained by Verlinde’s emergent gravity. This is the extension of Yoon et al. (2023), which examine the RAR of typical spiral galaxies, to less massive systems. To do this, we compile the line-of-sight velocity dispersion profiles of 30 dwarf galaxies in the Local Group from the literature. We then calculate the expected gravitational acceleration from the stellar component in the framework of the emergent gravity, and compare it with that from observations. The calculated acceleration with the emergent gravity under the assumption of a quasi-de Sitter universe agrees with the observed one within the uncertainty. Our results suggest that the emergent gravity can explain the kinematics of galaxies without introducing dark matter, even for less massive galaxies where dark matter is expected to dominate. This sharply contrasts with MOND, where a new interpolating function has to be introduced for dwarf galaxies to explain their kinematics without dark matter.

Introduction
Data and Method
    Properties and Stellar-Kinematic Data of Dwarf Spheroidal Galaxies
    Determination of Observed Gravitational Acceleration
    Prediction of the Gravitational Acceleration via Baryonic Components
Results
Discussion
Conclusions
Acknowledgments
References

• Sanghyeon Han(Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea)
• Ho Seong Hwang(Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea, SNU Astronomy Research Center, Seoul National University, Seoul 08826, Republic of Korea, Australian Astronomical Optics - Macquarie University, North Ryde NSW 2113, Australia) Corresponding author
• Youngsub Yoon(Department of Physics and Astronomy, Sejong University, Seoul 05006, Republic of Korea)