Resolved observations at 31 GHz of spinning dust emissivity variations in ρ Oph
Creators
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1.
University of Chile
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2.
Universidad Autónoma de Chile
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3.
University of Santiago Chile
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4.
University of Manchester
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5.
Princeton University
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6.
Instituto de Astrofísica de Canarias
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7.
University of La Laguna
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8.
Canadian Institute for Theoretical Astrophysics
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9.
University of Oxford
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10.
California Institute of Technology
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11.
Max Planck Institute for Radio Astronomy
Abstract
The ρ Oph molecular cloud is one of the best examples of spinning dust emission, first detected by the cosmic background imager (CBI). Here, we present 4.5 arcmin observations with CBI 2 that confirm 31 GHz emission from ρ Oph W, the PDR exposed to B-type star HD 147889, and highlight the absence of signal from S1, the brightest IR nebula in the complex. In order to quantify an association with dust-related emission mechanisms, we calculated correlations at different angular resolutions between the 31 GHz map and proxies for the column density of IR emitters, dust radiance, and optical depth templates. We found that the 31 GHz emission correlates best with the PAH column density tracers, while the correlation with the dust radiance improves when considering emission that is more extended (from the shorter baselines), suggesting that the angular resolution of the observations affects the correlation results. A proxy for the spinning dust emissivity reveals large variations within the complex, with a dynamic range of 25 at 3σ and a variation by a factor of at least 23, at 3σ, between the peak in ρ Oph W and the location of S1, which means that environmental factors are responsible for boosting spinning dust emissivities locally.
Additional Information
© 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2020 May 18. Received 2020 May 17; in original form 2019 October 13. Published: 22 May 2020. We thank the anonymous referee for helpful comments. CAT and SC acknowledge support from FONDECYT grant 1171624. MV acknowledges support from FONDECYT through grant 11191205. This work used the Brelka cluster (FONDEQUIP project EQM140101) hosted at DAS/U. de Chile. MC acknowledges support granted by CONICYT PFCHA/DOCTORADO BECAS CHILE/2018 - 72190574. CD was supported by an ERC Starting (Consolidator) grant (307209) under the FP7 and an STFC Consolidated grant (ST/P000649/1). This work was supported by the Strategic Alliance for the Implementation of New Technologies (SAINT, see www.astro.caltech.edu/chajnantor/saint/index.html), and we are most grateful to the SAINT partners for their strong support. We gratefully acknowledge support from B. Rawn and S. Rawn Jr. The CBI was supported by NSF grants 9802989, 0098734, and 0206416. This research has used data from the Herschel Gould Belt survey project (http://gouldbelt-herschel.cea.fr).Attached Files
Published - staa1422.pdf
Accepted Version - 1910.06359.pdf
Files
1910.06359.pdf
Additional details
Identifiers
- Eprint ID
- 104426
- Resolver ID
- CaltechAUTHORS:20200717-103452078
Related works
- Describes
- https://arxiv.org/abs/1910.06359 (URL)
Funding
- Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)
- 1171624
- Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)
- 11191205
- Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)
- 2018-72190574
- European Research Council (ERC)
- 307209
- Science and Technology Facilities Council (STFC)
- ST/P000649/1
- NSF
- AST-9802989
- NSF
- AST-0098734
- NSF
- AST-0206416
- NASA Spitzer Fellowship
Dates
- Created
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2020-07-17Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field
Caltech Custom Metadata
- Caltech groups
- Astronomy Department