NGC 4370: a case study for testing our ability to infer dust distribution and mass in nearby galaxies

Author: Viaene S.   De Geyter G.   Baes M.   Fritz J.   Bendo G. J.   Boquien M.   Boselli A.   Bianchi S.   Cortese L.   Côté P.   Cuillandre J.-C.   De Looze I.   di Serego Alighieri S.   Ferrarese L.   Gwyn S. D. J.   Hughes T. M.   Pappalardo C.  

Publisher: Edp Sciences

E-ISSN: 1432-0746|579|issue|A103-A103

ISSN: 0004-6361

Source: Astronomy & Astrophysics, Vol.579, Iss.issue, 2015-07, pp. : A103-A103

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Abstract

Context. A segment of the early-type galaxy population hosts a prominent dust lane, often decoupled from its stellar body. Methods of quantifying the dust content of these systems based on optical imaging data usually yield dust masses that are an order of magnitude lower than dust masses derived from the observed far-IR (FIR) emission. The discrepancy is often explained by invoking a diffuse dust component that is hard to trace in the UV or optical.