{"paper":{"title":"Diffuse Galactic Light in the Field of the Translucent High Galactic Latitude Cloud MBM32","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"B. A. Peterson, H. Sameshima, K. Kawara, N. Ienaka, S. Oyabu, T. Tsujimoto, Y. Matsuoka","submitted_at":"2013-03-05T06:14:14Z","abstract_excerpt":"We have conducted B, g, V, and R-band imaging in a 45x40 arcmin^2 field containing part of the high Galactic latitude translucent cloud MBM32, and correlated the intensity of diffuse optical light S_\\nu(\\lambda) with that of 100 micron emission S_\\nu(100um). A chi^2 minimum analysis is applied to fit a linear function to the measured correlation and derive the slope parameter b(\\lambda)= \\Delta S_\\nu(\\lambda) / \\Delta S_\\nu(100um) of the best-fit linear function. Compiling a sample by combining our b(\\lambda) and published ones, we show that the b(\\lambda) strength varies from cloud to cloud b"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1303.0938","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"}