{"paper":{"title":"Dust-Gas Scaling Relations and OH Abundance in the Galactic ISM","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Carl Heiles, Claire E. Murray, Di Li, Hiep Nguyen, J. R. Dawson, L. Bronfman, M.-A. Miville-Desch\\^enes, Ningyu Tang, N. M. McClure-Griffiths, R. Finger, Sne\\v{z}ana Stanimirovi\\'c, Steven J. Gibson, Thomas Troland","submitted_at":"2018-05-30T03:10:01Z","abstract_excerpt":"Observations of interstellar dust are often used as a proxy for total gas column density $N_\\mathrm{H}$. By comparing $\\textit{Planck}$ thermal dust data (Release 1.2) and new dust reddening maps from Pan-STARRS 1 and 2MASS (Green et al. 2018), with accurate (opacity-corrected) HI column densities and newly-published OH data from the Arecibo Millennium survey and 21-SPONGE, we confirm linear correlations between dust optical depth $\\tau_{353}$, reddening $E(B{-}V)$ and the total proton column density $N_\\mathrm{H}$ in the range (1$-$30)$\\times$10$^{20}$cm$^{-2}$, along sightlines with no molec"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1805.11787","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}