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    ZFIRE: GALAXY CLUSTER KINEMATICS, Hα STAR FORMATION RATES, AND GAS PHASE METALLICITIES OF XMM-LSS J02182-05102 AT ${z}_{\mathrm{cl}}=1.6233$

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    Issue Date
    2015-09-16
    Author
    Tran, Kim-Vy H.
    Nanayakkara, Themiya
    Yuan, Tiantian
    Kacprzak, Glenn G.
    Glazebrook, Karl
    Kewley, Lisa J.
    Momcheva, Ivelina
    Papovich, Casey J.
    Quadri, Ryan
    Rudnick, Gregory H.
    Publisher
    The American Astronomical Society
    Type
    Article
    Article Version
    Scholarly/refereed, publisher version
    Rights
    © 2015. The American Astronomical Society. All rights reserved.
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    Abstract
    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 $1.612\;\lt \;$ ${z}_{\mathrm{spec}}$ $\;\lt \;1.635$ defined by 33 members of which 20 are at R${}_{\mathrm{proj}}$ $\;\lt \;1$ Mpc. The cluster redshift and velocity dispersion are ${z}_{\mathrm{cl}}=1.6233\pm 0.0003$ and ${\sigma }_{\mathrm{cl}}=254\pm 50$ km s−1. We reach NIR line sensitivities of ~0.3 × 10−17 erg s−1 cm−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 ${M}_{\odot }\;{\mathrm{yr}}^{-1}$ (26 members; R${}_{\mathrm{proj}}$ $\;\lt \;2$ Mpc) and show that the elevated star formation in the cluster core (R${}_{\mathrm{proj}}$ $\;\lt \;0.25$ 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${}_{\mathrm{proj}}$ ~ 1 Mpc. However, we do not detect any environmental imprint when comparing attenuation and gas phase metallicities: the cluster galaxies show similar trends with ${M}_{\star }$ as to the field, e.g., more massive galaxies have larger stellar attenuation. IRC 0218's gas phase metallicity–${M}_{\star }$ relation (MZR) is offset to lower metallicities relative to $z\sim 0$ 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 (${\rm{\Delta }}t\sim 1$ Gyr): the MZR for both galaxy clusters are remarkably consistent with each other and virtually identical to several field surveys at $z\sim 2$.
    URI
    http://hdl.handle.net/1808/22206
    DOI
    https://doi.org/10.1088/0004-637X/811/1/28
    Collections
    • Physics & Astronomy Scholarly Works [1711]
    Citation
    Tran, K.-V. H., Nanayakkara, T., Yuan, T., Kacprzak, G. G., Glazebrook, K., Kewley, L. J., … Tomczak, A. (2015). ZFIRE: GALAXY CLUSTER KINEMATICS, H α STAR FORMATION RATES, AND GAS PHASE METALLICITIES OF XMM-LSS J02182-05102 AT ${z}_{\mathrm{cl}}=1.6233$ . The Astrophysical Journal, 811(1), 28. doi:10.1088/0004-637x/811/1/28

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    Contact KU ScholarWorks
    785-864-8983
    KU Libraries
    1425 Jayhawk Blvd
    Lawrence, KS 66045
    785-864-8983

    KU Libraries
    1425 Jayhawk Blvd
    Lawrence, KS 66045
    Image Credits
     

     

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