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High-resolution Observations of Molecular Lines in Arp 220: Kinematics, Morphology, and Limits on the Applicability of the Ammonia Thermometer

Zschaechner, Laura K. and Ott, Jürgen and Walter, Fabian and Meier, David S. and Momjian, Emmanuel and Scoville, Nick (2016) High-resolution Observations of Molecular Lines in Arp 220: Kinematics, Morphology, and Limits on the Applicability of the Ammonia Thermometer. Astrophysical Journal, 833 (1). Art. No. 41. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20161212-153120377

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Abstract

We observe Arp 220, the nearest ultra-luminous infrared galaxy, over 4 GHz in the K and Ka bands, providing constraints for the kinematics and morphology, and identifying molecular species on scales resolving both nuclei (0".6 or 230 pc). We detect multiple molecular species, including hydroxyl (OH ^2Π_(3/2)J = 9/2 F= 4-4; 5-5) in both cores, and tentatively detect H_2O(6_(15)-5_(23)) at ~21.84 GHz in both nuclei, indicating the likely presence of maser emission. The observed frequency range also contains metastable ammonia transitions from (J, K) = (1, 1)–(5, 5), as well as the (9, 9) inversion line; together, they are a well-known thermometer of dense molecular gas. Furthermore, the non-metastable (4, 2) and (10, 9), and possibly the (3, 1), lines are also detected. We apply a standard temperature analysis to Arp 220; however, the analysis is complicated in that standard local thermal equilibrium (LTE) assumptions do not hold. There are indications that a substantial fraction of ammonia could be in the non-metastable transitions, as opposed to only the metastable ones. Thus, the non-metastable transitions could be essential to constraining the temperature. We compare all of these data to ALMA observations of this source, confirming the outflow previously observed by other tracers in both nuclei.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.3847/1538-4357/833/1/41DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/833/1/41/metaPublisherArticle
https://arxiv.org/abs/1609.04824arXivDiscussion Paper
ORCID:
AuthorORCID
Zschaechner, Laura K.0000-0002-9919-8672
Walter, Fabian0000-0003-4793-7880
Scoville, Nick0000-0002-0438-3323
Additional Information:© 2016. The American Astronomical Society. Received 2015 October 29; revised 2016 September 9; accepted 2016 September 13; published 2016 December 6. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00175.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. The authors thank Brent Groves and Yancy Shirley for insightful discussions concerning ammonia properties and LVG analysis. We also thank Elizabeth Mills for insight concerning ammonia masers and column densities. Finally, we thank the anonymous referee for exceptionally insightful and relevant comments leading to substantial improvement of this manuscript.
Group:COSMOS
Subject Keywords:astrochemistry; galaxies: evolution; galaxies: individual (Arp 220) ; galaxies: ISM; galaxies: nuclei; galaxies: starburst
Record Number:CaltechAUTHORS:20161212-153120377
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20161212-153120377
Official Citation:Laura K. Zschaechner et al 2016 ApJ 833 41
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:72734
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:12 Dec 2016 23:47
Last Modified:20 Aug 2017 05:44

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