Zfire: Similar stellar growth in hα-emitting cluster and field galaxies at z ∼ 2

Article


Tran, Kim-Vy H., Alcorn, Leo Y., Kacprzak, Glenn G., Nanayakkara, Themiya, Straatman, Caroline, Yuan, Tiantian, Cowley, Michael, Davé, Romeel, Glazebrook, Karl, Kewley, Lisa J., Labbé, Ivo, Martizzi, Davidé, Papovich, Casey, Quadri, Ryan, Spitler, Lee R. and Tomczak, Adam. 2017. "Zfire: Similar stellar growth in hα-emitting cluster and field galaxies at z ∼ 2." The Astrophysical Journal: an international review of astronomy and astronomical physics. 834 (2), pp. 1-14. https://doi.org/10.3847/1538-4357/834/2/101
Article Title

Zfire: Similar stellar growth in hα-emitting cluster and field galaxies at z ∼ 2

ERA Journal ID1057
Article CategoryArticle
AuthorsTran, Kim-Vy H., Alcorn, Leo Y., Kacprzak, Glenn G., Nanayakkara, Themiya, Straatman, Caroline, Yuan, Tiantian, Cowley, Michael, Davé, Romeel, Glazebrook, Karl, Kewley, Lisa J., Labbé, Ivo, Martizzi, Davidé, Papovich, Casey, Quadri, Ryan, Spitler, Lee R. and Tomczak, Adam
Journal TitleThe Astrophysical Journal: an international review of astronomy and astronomical physics
Journal Citation834 (2), pp. 1-14
Article Number101
Number of Pages14
Year2017
PublisherIOP Publishing
Place of PublicationUnited States
ISSN0004-637X
1538-4357
Digital Object Identifier (DOI)https://doi.org/10.3847/1538-4357/834/2/101
Web Address (URL)https://iopscience.iop.org/article/10.3847/1538-4357/834/2/101
Abstract

We compare galaxy scaling relations as a function of environment at z ∼ 2 with our ZFIRE survey12 where we have measured Hα fluxes for 90 star-forming galaxies selected from a mass-limited (log(Mz.astModot) > 9) sample based on ZFOURGE.13 The cluster galaxies (37) are part of a confirmed system at z=2.095 and the field galaxies (53) are at 1.9 < z < 2.4; all are in the COSMOS legacy field. There is no statistical difference between Hα- emitting cluster and field populations when comparing their star formation rate (SFR), stellar mass (M∗), galaxy size (reff ), SFR surface density (σ(H star)), and stellar age distributions. The only difference is that at fixed stellar mass, the Hα-emitting cluster galaxies are log(reff ) ∼ 0.1 larger than in the field. Approximately 19% of the Hα-emitters in the cluster and 26% in the field are IR-luminous (LIR > 2>× 1011 L⊙). Because the luminous IR galaxies in our combined sample are ∼5 times more massive than the low-IR galaxies, their radii are ∼70% larger. To track stellar growth, we separate galaxies into those that lie above, on, or below the Hα star-forming main sequence (SFMS) using δSFR(M∗)=±0.2 dex. Galaxies above the SFMS (starbursts) tend to have higher Hα SFR surface densities and younger light-weighted stellar ages than galaxies below the SFMS. Our results indicate that starbursts (+SFMS) in the cluster and field at z ∼ 2 are growing their stellar cores. Lastly, we compare to the (SFR-M∗) relation from RHAPSODY-G cluster simulations and find that the predicted slope is nominally consistent with the observations. However, the predicted cluster SFRs tend to be too low by a factor of ∼2, which seems to be a common problem for simulations across environment.

Keywordsgalaxies: evolution; galaxies: star formation; galaxies: starburst
FunderDirectorate for Mathematical and Physical Sciences
Byline AffiliationsTexas A&M University, United States
Swinburne University of Technology
Leiden University, Netherlands
Australian National University
Macquarie University
Australian Astronomical Observatory, Australia
University of the Western Cape, South Africa
South African Astronomical Observatory, South Africa
African Institute for Mathematical Sciences, South Africa
University of California, United States
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