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The ALPINE-ALMA [CII] Survey: Kinematic Diversity & Rotation in Massive Star Forming Galaxies at z ~ 4.4-5.9

Jones, G. C. and Vergani, D. and Romano, M. and Ginolfi, M. and Fudamoto, Y. and Béthermin, M. and Fujimoto, S. and Lemaux, B. C. and Morselli, L. and Capak, P. and Cassata, P. and Faisst, A. and Le Fèvre, O. and Schaerer, D. and Silverman, J. D. and Yan, Lin and Boquien, M. and Cimatti, A. and Dessauges-Zavadsky, M. and Ibar, E. and Maiolino, R. and Rizzo, F. and Talia, M. and Zamorani, G. (2021) The ALPINE-ALMA [CII] Survey: Kinematic Diversity & Rotation in Massive Star Forming Galaxies at z ~ 4.4-5.9. . (Unpublished) https://resolver.caltech.edu/CaltechAUTHORS:20210412-131332609

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Abstract

Over the past decades, the kinematics of galaxies in the local Universe and at intermediate redshift (i.e., z~1-3) have been characterized in great detail, but only a handful of galaxies at high redshift (z>4) have been examined in such a way. The Atacama Large Millimeter/submillimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE) survey observed 118 star-forming main sequence galaxies at z = 4.4-5.9 in [CII]158um emission, increasing the number of such observations by nearly an order of magnitude. To characterize the morpho-kinematics of this sample, we apply a well-tested tilted ring model fitting code (^(3D)Barolo), a quantitative morphological classification (Gini-M₂₀), and a set of disk identification criteria to the ALPINE data. By exploring the G-M₂₀ of z>4 rest-frame FIR and [CII] data for the first time, we find that our 1"~6kpc resolution is insufficient to separate galaxy types based solely on these data. Of the 75 [CII]-detected ALPINE galaxies, 29 are detected at high enough significance and with sufficient spatial resolution to allow for tilted ring model fitting and the derivation of morpho-kinematic parameters. By combining these results with disk identification criteria, we are able to robustly classify 14 of the 29 fit sources (six rotators, five mergers, and three dispersion-dominated systems), with the remaining sources showing complex behaviour. We then compare the rotation curves and dynamical mass profiles of the six ALPINE rotators to the two previously detected z~4-6 unlensed main sequence rotators, finding high rotational velocities (~50-250km s⁻¹) and a range of rotation curve shapes.


Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/2104.03099arXivDiscussion Paper
ORCID:
AuthorORCID
Jones, G. C.0000-0002-0267-9024
Vergani, D.0000-0003-0898-2216
Romano, M.0000-0002-9948-3916
Ginolfi, M.0000-0002-8231-821X
Fudamoto, Y.0000-0001-7440-8832
Béthermin, M.0000-0002-3915-2015
Fujimoto, S.0000-0001-7201-5066
Lemaux, B. C.0000-0002-1428-7036
Morselli, L.0000-0003-0753-2571
Capak, P.0000-0003-3578-6843
Cassata, P.0000-0002-6716-4400
Faisst, A.0000-0002-9382-9832
Le Fèvre, O.0000-0001-5891-2596
Schaerer, D.0000-0001-7144-7182
Silverman, J. D.0000-0002-0000-6977
Yan, Lin0000-0003-1710-9339
Boquien, M.0000-0003-0946-6176
Cimatti, A.0000-0002-4409-5633
Dessauges-Zavadsky, M.0000-0003-0348-2917
Maiolino, R.0000-0002-4985-3819
Talia, M.0000-0003-4352-2063
Zamorani, G.0000-0002-2318-301X
Additional Information:Attribution 4.0 International (CC BY 4.0). This paper is based on data obtained with the ALMA Observatory, under Large Program 2017.1.00428.L. We also analyse archival data from ALMA programs 2012.1.00523.S and 2017.1.01052.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST 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. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This program is supported by the national program Cosmology and Galaxies from the CNRS in France. G.C.J. and R.M. acknowledge ERC Advanced Grant 695671 “QUENCH” and support by the Science and Technology Facilities Council (STFC). J.D.S. was supported by the JSPS KAKENHI Grant Number *JP18H04346*, and the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. A.C. and M.T. acknowledge the support from grant PRINMIUR 2017 - 20173ML3WW_001 This paper is dedicated to the memory of Olivier Le Fèvre, PI of the ALPINE survey. Data Availability: The data analysed in this work are available from the ALMA data archive (https://almascience.nrao.edu/asax/) under project code 2017.1.00428.L. Catalogs and data products are available from the ALPINE Data Release page (https://cesam.lam.fr/a2c2s/data_release.php).
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
European Research Council (ERC)695671
Science and Technology Facilities Council (STFC)UNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP18H04346
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)20173ML3WW_001
Subject Keywords:galaxies: evolution – galaxies: high-redshift – galaxies: kinematics and dynamics
Record Number:CaltechAUTHORS:20210412-131332609
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20210412-131332609
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108701
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:13 Apr 2021 21:35
Last Modified:23 Apr 2021 18:28

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