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Interpretation of radio continuum and molecular line observations of Sgr B2: free-free and synchrotron emission, and implications for cosmic rays

Protheroe, R. J. and Ott, J. and Ekers, R. D. and Jones, D. I. and Crocker, R. M. (2008) Interpretation of radio continuum and molecular line observations of Sgr B2: free-free and synchrotron emission, and implications for cosmic rays. Monthly Notices of the Royal Astronomical Society, 390 (2). pp. 683-692. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:PROmnras08

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Abstract

Recent ammonia (1,1) inversion line data on the Galactic star-forming region Sgr B2 show that the column density is consistent with a radial Gaussian density profile with a standard deviation of 2.75 pc. Deriving a formula for the virial mass of spherical Gaussian clouds, we obtain M_(vir) = 1.9 x 10^6 M⊙ for Sgr B2. For this matter distribution, a reasonable magnetic field and an impinging flux of cosmic rays of solar neighbourhood intensity, we predict the expected synchrotron emission from the Sgr B2 giant molecular cloud due to secondary electrons and positrons resulting from cosmic-ray interactions, including effects of losses due to pion production collisions during diffusive propagation into the cloud complex. We assemble radio-continuum data at frequencies between 330 MHz and 230 GHz. From the spectral-energy distribution, the emission appears to be thermal at all frequencies. Before using these data to constrain the predicted synchrotron flux, we first model the spectrum as free-free emission from the known ultra compact H II regions plus emission from an envelope or wind with a radial-density gradient, and obtain an excellent fit. We thus find the spectrum at all frequencies to be dominated by thermal emission, and this severely constrains the possible synchrotron emission by secondary electrons to quite low-flux levels. The absence of a significant contribution by secondary electrons is almost certainly due to multi-GeV energy cosmic rays being unable to penetrate far into giant molecular clouds. This would also explain why 100 MeV-GeV gamma-rays (from neutral pion decay or bremsstrahlung by secondary electrons) were not observed from Sgr B2 by the EGRET instrument on the Compton Gamma Ray Observatory, while TeV energy gamma-rays were observed by the High Energy Stereoscopic System (HESS), being produced by higher energy cosmic rays which more readily penetrate giant molecular clouds.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1111/j.1365-2966.2008.13752.xDOIArticle
ORCID:
AuthorORCID
Ott, J.0000-0001-8224-1956
Additional Information:© 2008 The Authors. Journal compilation © 2008 RAS. Accepted 2008 July 23. Received 2008 July 19; in original form 2008 June 16. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The ATCA is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research was supported under the Australian Research Council’s Discovery Project funding scheme (project number DP0559991). While this research was conducted Professor R. D. Ekers was the recipient of an Australian Research Council Federation Fellowship (project number FF0345330). The authors thank T. Stanev for providing particle physics data employed in this paper. We thank the referee for helpful comments.
Funders:
Funding AgencyGrant Number
Australian Research CouncilDP0559991
Australian Research CouncilFF0345330
Subject Keywords:radiation mechanisms: non-thermal; cosmic rays; HII regions; ISM: individual: Sgr B2 Giant Molecular Cloud; radio continuum: ISM; radio lines: ISM
Issue or Number:2
Record Number:CaltechAUTHORS:PROmnras08
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:PROmnras08
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:13408
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:08 May 2009 17:51
Last Modified:03 Oct 2019 00:37

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