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Resolved observations at 31 GHz of spinning dust emissivity variations in ρ Oph

Arce-Tord, Carla and Vidal, Matias and Casassus, Simon and Cárcamo, Miguel and Dickinson, Clive and Hensley, Brandon S. and Génova-Santos, Ricardo and Bond, J. Richard and Jones, Michael E. and Readhead, Anthony C. S. and Taylor, Angela C. and Zensus, J. Anton (2020) Resolved observations at 31 GHz of spinning dust emissivity variations in ρ Oph. Monthly Notices of the Royal Astronomical Society, 495 (3). pp. 3482-3493. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20200717-103452078

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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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/staa1422DOIArticle
https://arxiv.org/abs/1910.06359arXivDiscussion Paper
ORCID:
AuthorORCID
Arce-Tord, Carla0000-0002-0176-4331
Vidal, Matias0000-0003-2134-1587
Casassus, Simon0000-0002-0433-9840
Cárcamo, Miguel0000-0003-0564-8167
Dickinson, Clive0000-0002-0045-442X
Hensley, Brandon S.0000-0001-7449-4638
Génova-Santos, Ricardo0000-0001-5479-0034
Bond, J. Richard0000-0003-2358-9949
Jones, Michael E.0000-0003-3564-6680
Readhead, Anthony C. S.0000-0001-9152-961X
Zensus, J. Anton0000-0001-7470-3321
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).
Group:Astronomy Department
Funders:
Funding AgencyGrant Number
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
NSFAST-9802989
NSFAST-0098734
NSFAST-0206416
NASA Spitzer FellowshipUNSPECIFIED
Subject Keywords:radiationmechanisms: general – ISM: clouds – dust, extinction – ISM: individual objects: ρ Oph – photodissociation region – radio continuum: ISM
Issue or Number:3
Record Number:CaltechAUTHORS:20200717-103452078
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200717-103452078
Official Citation:Carla Arce-Tord, Matias Vidal, Simon Casassus, Miguel Cárcamo, Clive Dickinson, Brandon S Hensley, Ricardo Génova-Santos, J Richard Bond, Michael E Jones, Anthony C S Readhead, Angela C Taylor, J Anton Zensus, Resolved observations at 31 GHz of spinning dust emissivity variations in ρ Oph, Monthly Notices of the Royal Astronomical Society, Volume 495, Issue 3, July 2020, Pages 3482–3493, https://doi.org/10.1093/mnras/staa1422
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104426
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:17 Jul 2020 18:05
Last Modified:17 Jul 2020 18:05

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