Spitzer characterization of dust in an anomalous emission region: the Perseus cloud
Author
dc.contributor.author
Tibbs, C. T.
Author
dc.contributor.author
Flagey, N.
es_CL
Author
dc.contributor.author
Paladini, R.
es_CL
Author
dc.contributor.author
Compiègne, M.
es_CL
Author
dc.contributor.author
Shenoy, S.
es_CL
Author
dc.contributor.author
Carey, S.
es_CL
Author
dc.contributor.author
Noriega Crespo, A.
es_CL
Author
dc.contributor.author
Dickinson, C.
es_CL
Author
dc.contributor.author
Ali Haïmoud, Y.
es_CL
Author
dc.contributor.author
Casassus Montero, Simón
es_CL
Author
dc.contributor.author
Cleary, K.
es_CL
Author
dc.contributor.author
Davies, R. D.
es_CL
Author
dc.contributor.author
Hirata, C. M.
es_CL
Author
dc.contributor.author
Watson, R. A.
es_CL
Admission date
dc.date.accessioned
2014-01-08T19:58:20Z
Available date
dc.date.available
2014-01-08T19:58:20Z
Publication date
dc.date.issued
2011
Cita de ítem
dc.identifier.citation
Mon. Not. R. Astron. Soc. 418, 1889–1900 (2011)
en_US
Identifier
dc.identifier.other
doi:10.1111/j.1365-2966.2011.19605.x
Identifier
dc.identifier.uri
https://repositorio.uchile.cl/handle/2250/126080
General note
dc.description
Artículo de publicación ISI
en_US
Abstract
dc.description.abstract
Anomalous microwave emission is known to exist in the Perseus cloud. One of the most
promising candidates to explain this excess of emission is electric dipole radiation from
rapidly rotating very small dust grains, commonly referred to as spinning dust. Photometric
data obtained with the Spitzer Space Telescope have been reprocessed and used in conjunction
with the dust emission model DUSTEM to characterize the properties of the dust within the cloud.
This analysis has allowed us to constrain spatial variations in the strength of the interstellar
radiation field (χISRF), the mass abundances of the polycyclic aromatic hydrocarbons (PAHs)
and the very small grains (VSGs) relative to the big grains (YPAH and YVSG), the column density
of hydrogen (NH) and the equilibrium dust temperature (Tdust). The parameter maps of YPAH,
YVSG and χISRF are the first of their kind to be produced for the Perseus cloud, and we used
these maps to investigate the physical conditions in which anomalous emission is observed.
We find that in regions of anomalous emission the strength of the ISRF, and consequently the
equilibrium temperature of the dust, is enhanced while there is no significant variation in the
abundances of the PAHs and the VSGs or the column density of hydrogen. We interpret these
results as an indication that the enhancement in χISRF might be affecting the properties of the
small stochastically heated dust grains resulting in an increase in the spinning dust emission
observed at 33 GHz. This is the first time that such an investigation has been performed, and we
believe that this type of analysis creates a new perspective in the field of anomalous emission
studies, and represents a powerful new tool for constraining spinning dust models.