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Properties of Galactic Cirrus Clouds Observed by BOOMERANG

Veneziani, M. and Ade, P. A. R. and Bock, J. J. and Boscaleri, A. and Crill, B. P. and de Bernardis, P. and De Gasperis, G. and de Oliveira-Costa, A. and De Troia, G. and Di Stefano, G. and Ganga, K. M. and Jones, W. C. and Kisner, T. S. and Lange, A. E. and MacTavish, C. J. and Masi, S. and Mauskopf, P. D. and Montroy, T. E. and Natoli, P. and Netterfield, C. B. and Pascale, E. and Piacentini, F. and Pietrobon, D. and Polenta, G. and Ricciardi, S. and Romeo, G. and Ruhl, J. E. (2010) Properties of Galactic Cirrus Clouds Observed by BOOMERANG. Astrophysical Journal, 713 (2). pp. 959-969. ISSN 0004-637X.

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The physical properties of galactic cirrus emission are not well characterized. BOOMERANG is a balloon-borne experiment designed to study the cosmic microwave background at high angular resolution in the millimeter range. The BOOMERANG 245 and 345 GHz channels are sensitive to interstellar signals, in a spectral range intermediate between FIR and microwave frequencies. We look for physical characteristics of cirrus structures in a region at high galactic latitudes (b ~ –40°) where BOOMERANG performed its deepest integration, combining the BOOMERANG data with other available data sets at different wavelengths. We have detected eight emission patches in the 345 GHz map, consistent with cirrus dust in the Infrared Astronomical Satellite maps. The analysis technique we have developed allows us to identify the location and the shape of cirrus clouds, and to extract the flux from observations with different instruments at different wavelengths and angular resolutions. We study the integrated flux emitted from these cirrus clouds using data from Infrared Astronomical Satellite (IRAS), DIRBE, BOOMERANG and Wilkinson Microwave Anisotropy Probe in the frequency range 23-3000 GHz (13 mm-100 μm wavelength). We fit the measured spectral energy distributions with a combination of a gray body and a power-law spectra considering two models for the thermal emission. The temperature of the thermal dust component varies in the 7-20 K range and its emissivity spectral index is in the 1-5 range. We identified a physical relation between temperature and spectral index as had been proposed in previous works. This technique can be proficiently used for the forthcoming Planck and Herschel missions data.

Item Type:Article
Related URLs:
URLURL TypeDescription
Ade, P. A. R.0000-0002-5127-0401
Bock, J. J.0000-0002-5710-5212
Crill, B. P.0000-0002-4650-8518
de Bernardis, P.0000-0001-6547-6446
Masi, S.0000-0001-5105-1439
Mauskopf, P. D.0000-0001-6397-5516
Pascale, E.0000-0002-3242-8154
Piacentini, F.0000-0002-5444-9327
Additional Information:© 2010 American Astronomical Society. Received 2009 July 28; accepted 2010 March 1; published 2010 March 29. The authors acknowledge Jean-Philippe Bernard, Robert Crittenden, Alessandro Melchiorri and Max Tegmark for useful discussions. M.V. acknowledges support from the Faculty of the European Space Astronomy Center (ESAC-ESA). This activity has been supported by Italian Space Agency contracts COFIS, BOOMERanG and HiGal (I/038/08/0). We are grateful to the referee for helpful comments.
Funding AgencyGrant Number
Faculty of the European Space Astronomy Center (ESAC-ESA)UNSPECIFIED
Italian Space AgencyI/038/08/0
Subject Keywords:cosmology: observations; ISM: clouds; radio continuum: ISM; submillimeter: ISM
Issue or Number:2
Classification Code:PACS: 98.58.Ca; 98.70.Vc; 95.30.Wi; 98.80.-k
Record Number:CaltechAUTHORS:20100519-165135784
Persistent URL:
Official Citation:M. Veneziani et al 2010 ApJ 713 959 doi: 10.1088/0004-637X/713/2/959
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:18358
Deposited By: Jason Perez
Deposited On:20 May 2010 19:29
Last Modified:09 Mar 2020 13:19

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