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High-resolution Radio Continuum Measurements of the Nuclear Disks of Arp 220

Barcos-Muñoz, L. and Leroy, A. K. and Evans, A. S. and Privon, G. C. and Armus, L. and Condon, J. and Mazzarella, J. M. and Meier, D. S. and Momjian, E. and Murphy, E. J. and Ott, J. and Reichardt, A. and Sakamoto, K. and Sanders, D. B. and Schinnerer, E. and Stierwalt, S. and Surace, J. A. and Thompson, T. A. and Walter, F. (2015) High-resolution Radio Continuum Measurements of the Nuclear Disks of Arp 220. Astrophysical Journal, 799 (1). Art. No. 10. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20150226-153050963

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Abstract

We present new Karl G. Jansky Very Large Array radio continuum images of the nuclei of Arp 220, the nearest ultra-luminous infrared galaxy. These new images have both the angular resolution to study the detailed morphologies of the two nuclei that power the galaxy merger and sensitivity to a wide range of spatial scales. At 33 GHz, we achieve a resolution of 0."081 × 0."063 (29.9 × 23.3 pc) and resolve the radio emission surrounding both nuclei. We conclude from the decomposition of the radio spectral energy distribution that a majority of the 33 GHz emission is synchrotron radiation. The spatial distributions of radio emission in both nuclei are well described by exponential profiles. These have deconvolved half-light radii (R_(50d) ) of 51 and 35 pc for the eastern and western nuclei, respectively, and they match the number density profile of radio supernovae observed with very long baseline interferometry. This similarity might be due to the fast cooling of cosmic rays electrons caused by the presence of a strong (~mG) magnetic field in this system. We estimate extremely high molecular gas surface densities of 2.2^(+2.1)_(-1.0) x 10^5 (east) and 4.5^(+4.5)_(-1.9) x 10^5 (west) M_☉ pc^(–2), corresponding to total hydrogen column densities of N_H = 2.7^(+2.7)_(-1.2) x 10^(25) (east) and 5.6^(+5.5)_(-2.4) x 10^(25) cm^(–2) (west). The implied gas volume densities are similarly high, (n_(H_(_2)) ~ 3.8^(+3.8)_(-1.6) x 10^4 (east) and ~ 11^(+12)_(-4.5) x 10^4 cm^(–3) (west). We also estimate very high luminosity surface densities of ∑_(IR) ~ 4.2^(+1.6)_(-0.7) x 10^(13) (east) and ∑_(IR) ~ 9.7^(+3.7)_(-2.4) x 10^(13) (west) L_☉kpc^(-2), and star formation rate surface densities of Σ_(SFR) ~ 10^(3.7 ± 0.1) (east) and Σ_(SFR) ~ 10^(4.1 ± 0.1)(west) M_☉ yr^(–1)kpc^(–2). These values, especially for the western nucleus are, to our knowledge, the highest luminosity surface densities and star formation rate surface densities measured for any star-forming system. Despite these high values, the nuclei appear to lie below the dusty Eddington limit in which radiation pressure is balanced only by self-gravity. The small measured sizes also imply that at wavelengths shorter than λ = 1 mm, dust absorption effects must play an important role in the observed light distribution while below 5 GHz free-free absorption contributes substantial opacity. According to these calculations, the nuclei of Arp 220 are only transparent in the frequency range ~5-350 GHz. Our results offer no clear evidence that an active galactic nucleus dominates the emission from either nucleus at 33 GHz.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/799/1/10DOIArticle
http://iopscience.iop.org/0004-637X/799/1/10/PublisherArticle
http://arxiv.org/abs/1411.0932arXivDiscussion Paper
ORCID:
AuthorORCID
Barcos-Muñoz, L.0000-0003-0057-8892
Leroy, A. K.0000-0002-2545-1700
Privon, G. C.0000-0003-3474-1125
Condon, J.0000-0003-4724-1939
Mazzarella, J. M.0000-0002-8204-8619
Meier, D. S.0000-0001-9436-9471
Momjian, E.0000-0003-3168-5922
Murphy, E. J.0000-0001-7089-7325
Ott, J.0000-0001-8224-1956
Sakamoto, K.0000-0003-0494-8838
Sanders, D. B.0000-0002-1233-9998
Schinnerer, E.0000-0002-3933-7677
Surace, J. A.0000-0001-7291-0087
Walter, F.0000-0003-4793-7880
Additional Information:© 2015 American Astronomical Society. Received 2014 May 1; accepted 2014 November 3; published 2015 January 12. We thank the anonymous referee for helpful comments that made this paper stronger. We thank Guillermo Damke for his helpful input in the modeling process, Norman Murray for helpful discussions at an early stage of the project, Phil Arras for useful suggestions on Appendix A, and Shane Davis for his input, especially in the development of Appendix B, regarding radiation pressure and the Eddington limit. We thank the NRAO/UVa star formation group (especially Crystal Brogan and Kelsey Johnson) for repeated technical and scientific feedback. We also thank Nick Scoville for detailed discussions of the astrometry of Arp 220. A.S.E., G.C.P., and L.B.-M. were supported by NSF grant AST 1109475. L.B.-M. was also supported by Fulbright and Becas Chile—CONICYT. This research made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, and NASA’s Astrophysics Data System Bibliographic Services. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NSFAST-1109475
Fulbright FoundationUNSPECIFIED
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)UNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
NASA Astrophysics Data System Bibliographic ServicesUNSPECIFIED
Subject Keywords:galaxies: active; galaxies: individual (Arp 220); galaxies: interactions; galaxies: starburst; radio continuum: galaxies
Record Number:CaltechAUTHORS:20150226-153050963
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20150226-153050963
Official Citation:High-resolution Radio Continuum Measurements of the Nuclear Disks of Arp 220 L. Barcos-Muñoz et al. 2015 ApJ 799 10
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:55280
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:27 Feb 2015 20:22
Last Modified:02 Nov 2017 20:41

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