Antialigned spin of GW191109: Glitch mitigation and its implications

With a high total mass and an inferred effective spin antialigned with the orbital axis at the 99. 9% level, GW191109 is one of the most promising candidates for a dynamical formation origin among gravitational wave events observed so far. However, the data containing GW191109 are afflicted with terrestrial noise transients, i. e. , detector glitches, generated by the scattering of laser light in both LIGO detectors. We study the implications of the glitch (es) on the inferred properties and astrophysical interpretation of GW191109. Using time- and frequency-domain analysis methods, we isolate the critical data for spin inference to 35--40 Hz and 0. 1--0. 04 s before the merger in LIGO Livingston, directly coincident with the glitch. Using two models of glitch behavior, one tailored to slow scattered light and one more generic, we perform joint inference of the glitch and binary parameters. When the glitch is modeled as slow scattered light, the binary parameters favor antialigned spins, in agreement with existing interpretations. When more flexible glitch modeling based on sine-Gaussian wavelets is used instead, a bimodal aligned/antialigned solution emerges. The antialigned spin mode is correlated with a weaker inferred glitch and preferred by 70: 30 compared to the aligned spin mode and a stronger inferred glitch. We conclude that if we assume that the data are only impacted by slow scattering noise, then the antialigned spin inference is robust. However, the data alone cannot validate this assumption and resolve the antialigned spin and potentially dynamical formation history of GW191109.