2026ApJ...997..132S

We report on the H I content of an isolated, compact group of six dwarf galaxies at a distance of 145 Mpc. The distribution and kinematics of the H​​​​​​ I, including multiple gaseous bridges, indicate the group is a gravitationally bound system. The H I maps further reveal two newly discovered dwarf satellites easily identified by their gas but only barely visible in optical images. The four dwarf group members previously identified in the Sloan Digital Sky Survey have 9.06 < log(M_*/M_⊙) < 9.43 and 9.42 < log(M_H I_/M_⊙) < 9.73. The two newly discovered dwarf satellites have log(M_*/M_⊙) = 6.10 with log(M_H I_/M_⊙) = 8.71 and log(M_*/M_⊙) = 7.07 with log(M_H I_/M_⊙) = 9.18. New Gemini optical spectra link the H I detections and their optical counterparts. The group's 3D velocity dispersion (188 km s^–1), mass-to-light ratio (M/L_B ∼ 44), dynamical-to-baryonic mass ratio (M_dyn/M_bar ∼ 21), size (69 kpc), and gas fraction (0.56) are all consistent with the compact dwarf groups in the TNG50 simulation. The group has a top-heavy satellite mass function that is inconsistent with predictions for LMC-sized hosts and may instead be two or more groups coming together. A Voronoi tessellation reveals the group resides in a tendril outside the intersection of two filaments. These intermediate-density environments within the large-scale structure provide the conditions needed for groups of star-forming, gas-rich dwarf galaxies to form and eventually merge. Our results further show that it is possible to uncover fainter dwarf satellites around dwarf galaxy hosts via H I maps.