English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/109406
Share/Impact:
Statistics
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL | DATACITE
Exportar a otros formatos:

DC FieldValueLanguage
dc.contributor.authorBonaldi, A.-
dc.contributor.authorBarreiro, R. Belén-
dc.contributor.authorDiego, José María-
dc.contributor.authorGonzález-Nuevo, J.-
dc.contributor.authorToffolatti, L.-
dc.contributor.authorVielva, P.-
dc.contributor.authorRebolo López, Rafael-
dc.contributor.authorPlanck Collaboration-
dc.date.accessioned2015-01-15T12:34:39Z-
dc.date.available2015-01-15T12:34:39Z-
dc.date.issued2013-
dc.identifierdoi: 10.1051/0004-6361/201321160-
dc.identifierissn: 0004-6361-
dc.identifiere-issn: 1432-0746-
dc.identifier.citationAstronomy and Astrophysics 557: A53 (2013)-
dc.identifier.urihttp://hdl.handle.net/10261/109406-
dc.description.abstractWe perform an analysis of the diffuse low-frequency Galactic components in the southern part of the Gould Belt system (130◦ ≤ l ≤ 230◦ and −50◦ ≤ b ≤ −10◦). Strong ultra-violet flux coming from the Gould Belt super-association is responsible for bright diffuse foregrounds that we observe from our position inside the system and that can help us improve our knowledge of the Galactic emission. Free-free emission and anomalous microwave emission (AME) are the dominant components at low frequencies (ν < 40 GHz), while synchrotron emission is very smooth and faint. We separated diffuse free-free emission and AME from synchrotron emission and thermal dust emission by using Planck data, complemented by ancillary data, using the correlated component analysis (CCA) component-separation method and we compared our results with the results of cross-correlation of foreground templates with the frequency maps. We estimated the electron temperature Te from Hα and free-free emission using two methods (temperature-temperature plot and cross-correlation) and obtained Te ranging from 3100 to 5200 K for an effective fraction of absorbing dust along the line of sight of 30% ( fd = 0.3). We estimated the frequency spectrum of the diffuse AME and recovered a peak frequency (in flux density units) of 25.5±1.5 GHz.We verified the reliability of this result with realistic simulations that include biases in the spectral model for the AME and in the free-free template. By combining physical models for vibrational and rotational dust emission and adding the constraints from the thermal dust spectrum from Planck and IRAS, we are able to present a good description of the AME frequency spectrum for plausible values of the local density and radiation field.-
dc.description.sponsorshipThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU).-
dc.publisherEDP Sciences-
dc.relation.isversionofPublisher's version-
dc.rightsopenAccess-
dc.subjectGalaxy: general-
dc.subjectRadio continuum: ISM-
dc.subjectRadiation mechanisms: general-
dc.titlePlanck intermediate results: XII. Diffuse galactic components in the Gould Belt system-
dc.typeartículo-
dc.identifier.doi10.1051/0004-6361/201321160-
dc.relation.publisherversionhttp://dx.doi.org/10.1051/0004-6361/201321160-
dc.date.updated2015-01-15T12:34:39Z-
dc.description.versionPeer Reviewed-
dc.language.rfc3066eng-
Appears in Collections:(IFCA) Artículos
Files in This Item:
File Description SizeFormat 
XII. Diffuse Galactic.pdf9,19 MBAdobe PDFThumbnail
View/Open
Show simple item record
 

Related articles:


WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.