The MOSDEF Survey: Kinematic and Structural Evolution of Star-forming Galaxies at 1.4 ≤ z ≤ 3.8

Authors

• Sedona H. Price, Max Planck Institute for Extraterrestrial Physics
• Mariska Kriek, University of California, Berkeley
• Guillermo Barro, University of the PacificFollow
• Alice E. Shapley, University of California, Los Angeles
• Naveen A. Reddy, University of California, Riverside
• William R. Freeman, University of California, Riverside
• Alison L. Coil, Center for Astrophysics & Space Sciences
• Irene Shivaei, The University of Arizona
• Mojegan Azadi, Harvard-Smithsonian Center for Astrophysics
• Laura de Groot, The College of Wooster
• Brian Siana, University of California, Riverside
• Bahram Mobasher, University of California, Riverside
• Ryan L. Sanders, University of California, Davis
• Gene C.K. Leung, Center for Astrophysics & Space Sciences
• Tara Fetherolf, University of California, Riverside
• Tom O. Zick, University of California, Berkeley
• Hannah Übler, Max Planck Institute for Extraterrestrial Physics
• Natascha M. Förster Schreiber, Max Planck Institute for Extraterrestrial Physics

Document Type

Article

Publication Title

Astrophysical Journal

Department

Physics

ISSN

15384357

Volume

894

Issue

2

DOI

10.3847/1538-4357/ab7990

First Page

1

Last Page

26

Publication Date

5-8-2020

Abstract

We present ionized gas kinematics for 681 galaxies at z &tild; 1.4-3.8 from the MOSFIRE Deep Evolution Field survey, measured using models that account for random galaxy-slit misalignments together with structural parameters derived from CANDELS Hubble Space Telescope (HST) imaging. Kinematics and sizes are used to derive dynamical masses. Baryonic masses are estimated from stellar masses and inferred gas masses from dust-corrected star formation rates (SFRs) and the Kennicutt-Schmidt relation. We measure resolved rotation for 105 galaxies. For the remaining 576 galaxies we use models based on HST imaging structural parameters together with integrated velocity dispersions and baryonic masses to statistically constrain the median ratio of intrinsic ordered to disordered motion,. We find that increases with increasing stellar mass and decreasing specific SFR (sSFR). These trends may reflect marginal disk stability, where systems with higher gas fractions have thicker disks. For galaxies with detected rotation we assess trends between their kinematics and mass, sSFR, and baryon surface density (Σbar,e). Intrinsic dispersion correlates most with Σbar,e, and velocity correlates most with mass. By comparing dynamical and baryonic masses, we find that galaxies at z &tild; 1.4-3.8 are baryon dominated within their effective radii (RE), with Mdyn/Mbaryon increasing over time. The inferred baryon fractions within RE, fbar, decrease over time, even at fixed mass, size, or surface density. At fixed redshift, fbar does not appear to vary with stellar mass but increases with decreasing RE and increasing Σbar,e. For galaxies at z ≥ 2, the median inferred baryon fractions generally exceed 100%. We discuss possible explanations and future avenues to resolve this tension.

Creative Commons License

This work is licensed under a Creative Commons Attribution 4.0 International License.

Recommended Citation

Price, Sedona H.; Kriek, Mariska; Barro, Guillermo; Shapley, Alice E.; Reddy, Naveen A.; Freeman, William R.; Coil, Alison L.; Shivaei, Irene; Azadi, Mojegan; de Groot, Laura; Siana, Brian; Mobasher, Bahram; Sanders, Ryan L.; Leung, Gene C.K.; Fetherolf, Tara; Zick, Tom O.; Übler, Hannah; and Förster Schreiber, Natascha M., "The MOSDEF Survey: Kinematic and Structural Evolution of Star-forming Galaxies at 1.4 ≤ z ≤ 3.8" (2020). Pacific Faculty Work. 296.
https://scholarlycommons.pacific.edu/all-faculty/296