{"paper":{"title":"Determining dust temperatures and masses in the Herschel era: the importance of observations longward of 200 micron","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Bolatto, A.G.G.M. Tielens, A. Hughes, A. Li, C. Bot, C. Engelbracht, F. Galliano, F. Kemper, F. P. Israel, J.-P. Bernard, J. Roman-Duval, K. D. Gordon, K. Misselt, K. Okumura, M. Matsuura, M. Meixner, M. Rubio, M. Sauvage, P. Panuzzo, R. Skibba, S. C. Madden, S. Hony, S. Kim, W. T. Reach","submitted_at":"2010-05-14T11:01:14Z","abstract_excerpt":"The properties of the dust grains (e.g., temperature and mass) can be derived from fitting far-IR SEDs (>100 micron).  Only with SPIRE on Herschel has it been possible to get high spatial resolution at 200 to 500 micron that is beyond the peak (~160 micron) of dust emission in most galaxies.  We investigate the differences in the fitted dust temperatures and masses determined using only <200 micron data and then also including >200 micron data (new SPIRE observations) to determine how important having >200 micron data is for deriving these dust properties.  We fit the 100 to 350 micron observa"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1005.2497","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"}