CaltechAUTHORS
Published November 2021 | Version Submitted + Published
Journal Article Open

The ALPINE-ALMA [C II] Survey: kinematic diversity and rotation in massive star-forming galaxies at z ~ 4.4–5.9

Creators

  • 1. ROR icon University of Cambridge
  • 2. ROR icon University of Padua
  • 3. ROR icon European Southern Observatory
  • 4. ROR icon Waseda University
  • 5. ROR icon National Astronomical Observatory of Japan
  • 6. ROR icon Aix-Marseille University
  • 7. ROR icon University of Copenhagen
  • 8. ROR icon University of California, Berkeley
  • 9. ROR icon Infrared Processing and Analysis Center
  • 10. ROR icon University of Geneva
  • 11. ROR icon Kavli Institute for the Physics and Mathematics of the Universe
  • 12. ROR icon University of Tokyo
  • 13. ROR icon California Institute of Technology
  • 14. ROR icon University of Antofagasta
  • 15. ROR icon University of Bologna
  • 16. ROR icon Arcetri Astrophysical Observatory
  • 17. ROR icon University of Valparaíso

Abstract

While the kinematics of galaxies up to z ∼ 3 have been characterized in detail, 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 [C II] at Early times (ALPINE) survey observed a statistically significant sample of 118 star-forming main-sequence galaxies at z = 4.4–5.9 in [C II]158 μμm emission, increasing the number of such observations by nearly 10×. A preliminary qualitative classification of these sources revealed a diversity of kinematic types (i.e. rotators, mergers, and dispersion-dominated systems). In this work, we supplement the initial classification by applying quantitative analyses to the ALPINE data: a tilted ring model (TRM) fitting code (^(3D)BAROLO), a morphological classification (Gini-M₂₀), and a set of disc identification criteria. Of the 75 [C II]-detected ALPINE galaxies, 29 are detected at sufficient significance and spatial resolution to allow for TRM fitting and the derivation of morphological and kinematic parameters. These 29 sources constitute a high-mass subset of the ALPINE sample (⁠M∗ > 10^(9.5) M_⊙). We robustly classify 14 of these sources (six rotators, five mergers, and three dispersion-dominated systems); the remaining sources showing complex behaviour. By exploring the G-M₂₀ of z > 4 rest-frame far-infrared and [C II] data for the first time, we find that our 1 arcsec ∼ 6 kpc resolution data alone are insufficient to separate galaxy types. We 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 (∼50–250 km s⁻¹) and a diversity of rotation curve shapes.

Additional Information

© 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2021 July 29. Received 2021 July 29; in original form 2021 April 7. Published: 09 August 2021. We thank the anonymous referee for useful feedback that resulted in an improved manuscript. 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. GCJ and RM acknowledge ERC Advanced Grant 695671 'QUENCH' and support by the Science and Technology Facilities Council (STFC). JDS was supported by the JSPS KAKENHI Grant Number *JP18H04346*, and the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. AC and MT acknowledge the support from grant PRIN MIUR 2017 − 20173ML3WW_001. EI acknowledges partial support from FONDECYT through grant N○ 1171710. 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. Catalogues and data products are available from the ALPINE Data Release page (https://cesam.lam.fr/a2c2s/data_release.php).

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Published - stab2226.pdf

Submitted - 2104.03099.pdf

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2104.03099.pdf

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Additional details

Identifiers

Eprint ID
108701
Resolver ID
CaltechAUTHORS:20210412-131332609

Related works

Describes
https://arxiv.org/abs/2104.03099 (URL)
https://almascience.nrao.edu/asax (URL)
https://cesam.lam.fr/a2c2s/data_release.php (URL)

Funding

Centre National de la Recherche Scientifique (CNRS)
European Research Council (ERC)
695671
Science and Technology Facilities Council (STFC)
Japan Society for the Promotion of Science (JSPS)
JP18H04346
Ministry of Education, Culture, Sports, Science and Technology (MEXT)
Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)
20173ML3WW_001
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)
1171710

Dates

Created
2021-04-13
Created from EPrint's datestamp field
Updated
2021-10-26
Created from EPrint's last_modified field

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Caltech groups
Infrared Processing and Analysis Center (IPAC)