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A multi-wavelength investigation of RCW175: an H_II region harboring spinning dust emission

Tibbs, C. T. and Paladini, R. and Compiegne, M. and Dickinson, C. and Alves, M. I. R. and Flagey, N. and Shenoy, S. and Noriega-Crespo, A. and Carey, S. and Casassus, S. and Davies, R. D. and Davis, R. J. and Molinari, S. and Elia, D. and Pestalozzi, M. and Schisano, E. (2012) A multi-wavelength investigation of RCW175: an H_II region harboring spinning dust emission. Astrophysical Journal, 754 (2). Art. No. 94. ISSN 0004-637X.

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Using infrared, radio continuum and spectral observations, we performed a detailed investigation of the Hii region RCW175. We determined that RCW175, which actually consists of two separate Hii regions, G29.1-0.7 and G29.0-0.6, is located at a distance of 3.2 ± 0.2 kpc. Based on the observations we infer that the more compact G29.0-0.6 is less evolved than G29.1-0.7 and was possibly produced as a result of the expansion of G29.1-0.7 into the surrounding interstellar medium. We compute a star formation rate for RCW175 of (12.6 ± 1.9) x 10^(-5) M_⊙ yr^(-1), and identified 6 possible young stellar object candidates within its vicinity. Additionally, we estimate that RCW175 contains a total dust mass of 215 ± 53 M_⊙. RCW175 has previously been identified as a source of anomalous microwave emission (AME), an excess of emission at cm wavelengths often attributed to electric dipole radiation from the smallest dust grains. We find that the AME previously detected in RCW175 is not correlated with the smallest dust grains (polycyclic aromatic hydrocarbons or small carbonaceous dust grains), but rather with the exciting radiation field within the region. This is a similar result to that found in the Perseus molecular cloud, another region which harbors AME, suggesting that the radiation field may play a pivotal role in the production of this new Galactic emission mechanism. Finally, we suggest that these observations may hint at the importance of understanding the role played by the major gas ions in spinning dust models.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Paladini, R.0000-0002-5158-243X
Dickinson, C.0000-0002-0045-442X
Flagey, N.0000-0002-8763-1555
Noriega-Crespo, A.0000-0002-6296-8960
Carey, S.0000-0002-0221-6871
Additional Information:© 2012 The American Astronomical Society. Received 2012 March 18; accepted 2012 May 17; published 2012 July 12. We thank the anonymous referee for providing useful comments that improved the content of this paper. We also thank Mark Calabretta and Lister Staveley-Smith for help with the RRL data. This work has been performed within the framework of a NASA/ADP ROSES-2009 grant No. 09-ADP09-0059. C.D. acknowledges an STFC Advanced Fellowship and EU Marie Curie IRG grant under the FP7. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This publication makes use of molecular line data from the Boston University-FCRAO Galactic Ring Survey (GRS). The GRS is a joint project of Boston University and Five College Radio Astronomy Observatory, funded by the National Science Foundation under grants AST-9800334, AST-0098562, AST-0100793, AST-0228993, and AST-0507657. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven,CSL, IMEC (Belgium); CEA, LAM (France);MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA).
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)UNSPECIFIED
Marie Curie FellowshipUNSPECIFIED
Subject Keywords:dust, extinction – Hii regions – ISM: abundances – ISM: individual objects (RCW175, G29.1-0.7, G29.0-0.6)
Issue or Number:2
Record Number:CaltechAUTHORS:20120604-081346731
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Official Citation:A Multi-wavelength Investigation of RCW175: An H II Region Harboring Spinning Dust Emission C. T. Tibbs et al. 2012 ApJ 754 94
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:31788
Deposited By: Tony Diaz
Deposited On:31 Jul 2012 21:12
Last Modified:09 Mar 2020 13:19

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