{ "id": "2408.03136", "version": "v1", "published": "2024-08-06T12:23:58.000Z", "updated": "2024-08-06T12:23:58.000Z", "title": "A Dust-Scattering Model for M1-92: A Revised Estimate of the Mass Distribution and Inclination", "authors": [ "Yun Qi Li", "Mark R. Morris", "Raghvendra Sahai" ], "comment": "21 pages, 8 figures, accepted for publications in Galaxies", "journal": "Galaxies 2024, 12(4), 44", "doi": "10.3390/galaxies12040044", "categories": [ "astro-ph.SR", "astro-ph.GA" ], "abstract": "Preplanetary nebulae (PPNe) are formed from mass-ejecting late-stage AGB stars. Much of the light from the star gets scattered or absorbed by dust particles, giving rise to the observed reflection nebula seen at visible and near-IR wavelengths. Precursors to planetary nebulae (PNe), PPNe generally have not yet undergone any ionization by UV radiation from the still-buried stellar core. Bipolar PPNe are a common form of observed PPNe. This study lays the groundwork for future dynamical studies by reconstructing the dust density distribution of a particularly symmetric bipolar PPN, M1-92 (Minkowski's Footprint, IRAS 19343$+$2926). For this purpose, we develop an efficient single-scattering radiative transfer model with corrections for double-scattering. Using a V-band image from the Hubble Space Telescope (HST), we infer the dust density profile and orientation of M1-92. These results indicate that M1-92's slowly expanding equatorial torus exhibits an outer radial cutoff in its density, which implicates the influence of a binary companion during the formation of the nebula.", "revisions": [ { "version": "v1", "updated": "2024-08-06T12:23:58.000Z" } ], "analyses": { "keywords": [ "mass distribution", "dust-scattering model", "revised estimate", "single-scattering radiative transfer model", "inclination" ], "tags": [ "journal article" ], "note": { "typesetting": "TeX", "pages": 21, "language": "en", "license": "arXiv", "status": "editable" } } }