7662 20251226131057.0 SCART-2025-0153 Goldman, S.R. Equatorial Enhancement in the Dustiest OH/IR Stars in the Galactic Bulge 2025 We have detected the 10 μm silicate feature and the 11.3 μm crystalline forsterite feature in absorption in 21 oxygen-rich asymptotic giant branch stars in the Galactic bulge. The depths of the 10 μm feature indicate We have detected the 10 μm silicate feature and the 11.3 μm crystalline forsterite feature in absorption in 21 oxygen-rich asymptotic giant branch stars in the Galactic bulge. The depths of the 10 μm feature indicate highly obscured circumstellar environments. The additional crystalline features may suggest either an extended envelope or dust formation in a high-density environment. We have also modeled the spectral energy distributions (SEDs) of the sample using radiative transfer models, and compared the results to wind speeds measured using 1612 MHz circumstellar OH masers, as well as previous estimates of circumstellar properties. The 16 sources with measured pulsation periods appear on sequence D of the mid-IR period–luminosity relation, associated with the long secondary period. We suspect that all of these sources are in fact fundamental-mode pulsators. At least two sources appear on the fundamental-mode sequence when accounting for the dust content. For the remainder, these sources are also likely fundamental-mode pulsators with extended envelopes. Taken as a whole, the high optical depths, crystalline features, discrepancies between observed and modeled wind speeds, pulsation periods longer than other fundamental-mode pulsators, and SED and pulsation properties similar to those with known equatorially enhanced circumstellar envelopes (e.g., OH 26.5+0.6 and OH 30.1–0.7) lead us to believe that these sources are likely to be equatorially enhanced, highly obscured circumstellar environments. The additional crystalline features may suggest either an extended envelope or dust formation in a high-density environment. We have also modeled the spectral energy distributions (SEDs) of the sample using radiative transfer models, and compared the results to wind speeds measured using 1612 MHz circumstellar OHmasers, as well as previous estimates of circumstellar properties. The 16 sources with measured pulsation periods appear on sequence D of the mid-IR period–luminosity relation, associated with the long secondary period. We suspect that all of these sources are in fact fundamental-mode pulsators. At least two sources appear on the fundamental-mode sequence when accounting for the dust content. For the remainder, these sources are also likely fundamental-mode pulsators with extended envelopes. Taken as a whole, the high optical depths, crystalline features, discrepancies between observed and modeled wind speeds, pulsation periods longer than other fundamental-mode pulsators, and SED and pulsation properties similar to those with known equatorially enhanced circumstellar envelopes (e.g., OH 26.5+0.6 and OH 30.1–0.7) lead us to believe that these sources are likely to be equatorially enhanced. NO Galactic bulge Stellar mass loss Asymptotic giant branch stars Stellar winds Circumstellar dust Long period variable stars van Loon, J.Th. Jones, O.C. Blommaert, J.A.D.L Groenewegen, M.A.T. astrophysical journal 980 2025 191 martin.groenewegen@ksb-orb.be 1301820 http://publi2-as.oma.be/record/7662/files/GoldmanvanLoon_ea_25ApJ_980_191_Dustiest_OHIR_GalacricBulge.pdf 3677 http://publi2-as.oma.be/record/7662/files/GoldmanvanLoon_ea_25ApJ_980_191_Dustiest_OHIR_GalacricBulge.gif?subformat=icon icon 7021 http://publi2-as.oma.be/record/7662/files/GoldmanvanLoon_ea_25ApJ_980_191_Dustiest_OHIR_GalacricBulge.jpg?subformat=icon-180 icon-180 published in REFERD