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Dynamical Characterization of Galaxies at z ∼ 4–6 via Tilted Ring Fitting to ALMA [C II] Observations

Jones, G. C. and Carilli, C. L. and Shao, Y. and Wang, R. and Capak, P. L. and Pavesi, R. and Riechers, D. A. and Karim, A. and Neeleman, M. and Walter, F. (2017) Dynamical Characterization of Galaxies at z ∼ 4–6 via Tilted Ring Fitting to ALMA [C II] Observations. Astrophysical Journal, 850 (2). Art. No. 180. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20171130-124108209

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Abstract

Until recently, determining the rotational properties of galaxies in the early universe (z > 4, universe age <1.5 Gyr) was impractical, with the exception of a few strongly lensed systems. Combining the high resolution and sensitivity of ALMA at (sub-)millimeter wavelengths with the typically high strength of the [C II] 158 μm emission line from galaxies and long-developed dynamical modeling tools raises the possibility of characterizing the gas dynamics in both extreme starburst galaxies and normal star-forming disk galaxies at z ~ 4-7. Using a procedure centered around GIPSY's ROTCUR task, we have fit tilted ring models to some of the best available ALMA [C II] data of a small set of galaxies: the MS galaxies HZ9 and HZ10, the damped Lyα absorber host galaxy ALMA J0817+1351, the submm galaxies AzTEC/C159 and COSMOS J1000+0234, and the quasar host galaxy ULAS J1319+0950. This procedure directly derives rotation curves and dynamical masses as functions of radius for each object. In one case, we present evidence for a dark matter halo of O(10^(11))M⊙. We present an analysis of the possible velocity dispersions of two sources based on matching simulated observations to the integrated [C II] line profiles. Finally, we test the effects of observation resolution and sensitivity on our results. While the conclusions remain limited at the resolution and signal-to-noise ratios of these observations, the results demonstrate the viability of the modeling tools at high redshift, and the exciting potential for detailed dynamical analysis of the earliest galaxies, as ALMA achieves full observational capabilities.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa8df2DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa8df2/metaPublisherArticle
https://arxiv.org/abs/1709.04954arXivDiscussion Paper
ORCID:
AuthorORCID
Jones, G. C.0000-0002-0267-9024
Carilli, C. L.0000-0001-6647-3861
Capak, P. L.0000-0003-3578-6843
Pavesi, R.0000-0002-2263-646X
Riechers, D. A.0000-0001-9585-1462
Karim, A.0000-0002-8414-9579
Walter, F.0000-0003-4793-7880
Additional Information:© 2017 The American Astronomical Society. Received 2017 May 23; revised 2017 September 7; accepted 2017 September 14; published 2017 November 30. This work makes use of the following ALMA data: 2011.0.00206.S, 2012.1.00240.S, 2012.1.00523.S, 2012.1.00978.S, and 2015.1.01564.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and 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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. G.J. is grateful for support from NRAO through the Grote Reber Doctoral Fellowship Program. Y.S. acknowledges support from the China Scholarship Council. R.W. acknowledges support from the National Key Research and Development Program of China (2016YFA0400703), the Thousand Youth Talents Program of China, and the National Science Foundation of China (NSFC) grant No. 11473004. D.R. and R.P. acknowledge support from the National Science Foundation under grant number AST-1614213 to Cornell University. R.P. acknowledges support through award SOSPA3-008 from the NRAO. A.K. acknowledges support by the Collaborative Research Center 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG).
Group:COSMOS, Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
National Radio Astronomy ObservatoryUNSPECIFIED
China Scholarship CouncilUNSPECIFIED
National Key Research and Development Program of China2016YFA0400703
Thousand Youth Talents Program of ChinaUNSPECIFIED
National Natural Science Foundation of China11473004
NSFAST-1614213
Deutsche Forschungsgemeinschaft (DFG)956
Subject Keywords:galaxies: high-redshift – galaxies: kinematics and dynamics
Record Number:CaltechAUTHORS:20171130-124108209
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20171130-124108209
Official Citation:G. C. Jones et al 2017 ApJ 850 180
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:83601
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:30 Nov 2017 21:21
Last Modified:12 Jul 2019 17:25

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