ZFIRE: Galaxy cluster kinematics, Hα star formation rates, and gas phase metallicities of XMM-LSS J02182-05102 AT z{sub cl}=1.6233

Journal Article · Sun Sep 20 04:00:00 EDT 2015 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/811/1/28· OSTI ID:22882624

Tran, Kim-Vy H.; Papovich, Casey J.; Quadri, Ryan; Tomczak, Adam ^[1]; Nanayakkara, Themiya; Kacprzak, Glenn G.; Glazebrook, Karl ^[2]; Yuan, Tiantian; Kewley, Lisa J. ^[3]; Momcheva, Ivelina ^[4]; Rudnick, Greg ^[5]; Saintonge, Amélie ^[6]; Spitler, Lee R. ^[7]; Straatman, Caroline ^[8]

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1. George P. and Cynthia W. Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A and M University, College Station, TX 77843 (United States)
2. Swinburne University of Technology, Hawthorn, VIC 3122 (Australia)
3. Research School of Astronomy and Astrophysics, The Australian National University, Cotter Road, Weston Creek, ACT 2611 (Australia)
4. Astronomy Department, Yale University, New Haven, CT 06511 (United States)
5. Department of Physics and Astronomy, The University of Kansas, Malott Room 1082, 1251 Wescoe Hall Drive, Lawrence, KS 66045 (United States)
6. Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT (United Kingdom)
7. Department of Physics and Astronomy, Faculty of Science and Engineering, Macquarie University, Sydney, NSW 2109 (Australia)
8. Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden (Netherlands)

We spectroscopically survey the galaxy cluster XMM-LSS J02182-05102 (hereafter IRC 0218) using LRIS (optical) and MOSFIRE (near-infrared) on Keck I as part of the ZFIRE survey. IRC 0218 has a narrow redshift range of 1.612 < z{sub spec} < 1.635 defined by 33 members of which 20 are at R{sub proj} < 1 Mpc. The cluster redshift and velocity dispersion are z{sub cl}=1.6233±0.0003 and σ{sub cl}=254±50 km s{sup −1}. We reach NIR line sensitivities of ∼0.3 × 10{sup −17} erg s{sup −1} cm{sup −2} that, combined with multi-wavelength photometry, provide extinction-corrected Hα star formation rates (SFR), gas phase metallicities from [N ii]/Hα, and stellar masses. We measure an integrated Hα SFR of ∼325 M{sub ⊙} yr{sup −1} (26 members; R{sub proj} < 2 Mpc) and show that the elevated star formation in the cluster core (R{sub proj} < 0.25 Mpc) is driven by the concentration of star-forming members, but the average SFR per Hα-detected galaxy is half that of members at R{sub proj} ∼ 1 Mpc. However, we do not detect any environmental imprint when comparing attenuation and gas phase metallicities: the cluster galaxies show similar trends with M{sub ⋆} as to the field, e.g., more massive galaxies have larger stellar attenuation. IRC 0218’s gas phase metallicity–M{sub ⋆} relation (MZR) is offset to lower metallicities relative to z∼0 and has a slope of 0.13 ± 0.10. Comparing the MZR in IRC 0218 to the COSMOS cluster at z = 2.1 shows no evolution (Δt∼1 Gyr): the MZR for both galaxy clusters are remarkably consistent with each other and virtually identical to several field surveys at z∼2.

• OSTI ID: 22882624
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 811; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United Kingdom
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
COMPARATIVE EVALUATIONS
DISPERSIONS
GALACTIC EVOLUTION
GALAXIES
GALAXY CLUSTERS
MASS
METALLICITY
PHOTOMETRY
RED SHIFT
SENSITIVITY
STARS
UNIVERSE
VELOCITY