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Dust in dwarf galaxies: The case of NGC 4214

Published online by Cambridge University Press:  17 August 2012

U. Lisenfeld
Affiliation:
Universidad Granada, Granada, Spain, email: ute@ugr.es, mrelano@ugr.es, israelhermelo@ugr.es
I. Hermelo
Affiliation:
Universidad Granada, Granada, Spain, email: ute@ugr.es, mrelano@ugr.es, israelhermelo@ugr.es
M. Relaño
Affiliation:
Universidad Granada, Granada, Spain, email: ute@ugr.es, mrelano@ugr.es, israelhermelo@ugr.es
R. J. Tuffs
Affiliation:
Max-Planck-Institut für Kernphysik, Heidelberg, Germany, email: Richard.Tuffs@mpi-hd.mpg.de
C. C. Popescu
Affiliation:
Jeremiah Horrocks Institute for Astrophysics and Supercomputing, University of Central Lancashire, Prestion, U.K., email: cpopescu@uclan.ac.uk
J. Fischera
Affiliation:
Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto, email: fischera@cita.utoronto.ca
B. Groves
Affiliation:
Max-Planck-Institut für Astronomie, Heidelberg, Germany, email: brent@mpia.de
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Abstract

We have carried out a detailed modelling of the dust heating and emission in the nearby, starbursting dwarf galaxy NGC 4214. Due to its proximity and the great wealth of data from the UV to the millimeter range (from GALEX, HST, Spitzer, Herschel, Planck and IRAM) it is possible to separately model the emission from HII regions and their associated photodissociation regions (PDRs) and the emission from diffuse dust. Furthermore, most model parameters can be directly determined from the data leaving very few free parameters. We can fit both the emission from HII+PDR regions and the diffuse emission in NGC 4214 with these models with “normal” dust properties and realistic parameters.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2012

References

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