Exploring the Relationship between Swift Short Gamma-Ray Burst Afterglows and Their Host Galaxy Properties

Abstract We present a comprehensive compilation of short-duration γ -ray burst (GRB) afterglows in the X-ray, optical, and radio bands, comprising 111 events with detected afterglows discovered primarily by the Neil Gehrels Swift Observatory over 2005–2023. We pair these observations with uniformly modeled host galaxies to understand how broadband afterglow luminosities are influenced by their environmental properties. We compare the X-ray and optical afterglow luminosities at 3 hr with projected physical and host-normalized galactocentric offsets, host stellar mass, star formation rate (SFR), specific SFR, and stellar population age. In the radio band, we explore how these environmental properties may influence afterglow detectability. We find statistical support that X-ray afterglows are brighter in galaxies with younger ages, lower masses, and higher active star formation—trends that also scale with interstellar medium density. While we also visualize these differences for optical afterglows; the only statistically significant trend is that they are brighter in hosts with higher SFR. We further find that X-ray (radio) afterglows are more luminous (more likely to be detected) at low projected offsets. Overall, this indicates that X-ray afterglow luminosity aligns with most expectations among the three bands. We find the afterglow luminosities of three possible merger-driven long GRBs to be unremarkable compared to the traditional short GRB population, strengthening the case that these events arise from mergers. Finally, we find that the estimated on-axis afterglow luminosity of GW170817 is in the faintest ≈30%, aligning with its quiescent, old, and massive host environment.