Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 720394.0, MPI für Astronomie / Publikationen_mpia
High-resolution radio continuummeasurements of the nuclear disks of Arp 220
Authors:Barcos-Muñoz, L.; Leroy, A. K.; Evans, A. S.; Privon, G. C.; Armus, L.; Condon, J.; Mazzarella, J. M.; Meier, D. S.; Momjian, E.; Murphy, E. J.; Ott, J.; Reichardt, A.; Sakamoto, K.; Sanders, D. B.; Schinnerer, E.; Stierwalt, S.; Surace, J. A.; Thompson, T. A.; Walter, F.
Date of Publication (YYYY-MM-DD):2015
Title of Journal:The Astrophysical Journal
Issue / Number:1
Start Page:id. 10 (14 pp)
Audience:Not Specified
Abstract / Description: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 × 10^5 (east) and 4.5+4.5-1.9 × 10^5 (west) M pc-2, corresponding to total hydrogen column densities of N H = 2.7+2.7-1.2 × 1025 (east) and 5.6+5.5-2.4 × 1025 cm-2 (west). The implied gas volume densities are similarly high, {nH_{_2} ˜ 3.8+3.8-1.6 × 10^4} (east) and {˜ } 11+12-4.5 × 10^4 cm-3 (west). We also estimate very high luminosity surface densities of Σ _IR ˜ 4.2+1.6-0.7 × 1013 (east) and Σ _IR ˜ 9.7+3.7-2.4 × 1013 (west) L kpc-2, and star formation rate surface densities of ΣSFR ~ 103.7 ± 0.1 (east) and ΣSFR ~ 104.1 ± 0.1(west) M yr-1kpc-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.
Free Keywords:galaxies: active; galaxies: individual: Arp 220; galaxies: interactions; galaxies: starburst; radio continuum: galaxies
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-637X %R 10.1088/0004-637X/799/1/10
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.