ZFIRE: galaxy cluster kinematics, Hα star formation rates, and gas phase metallicities of XMM-LSS J02182-05102 at zcl=1.6233

Kim Vy H Tran; Themiya Nanayakkara; Tiantian Yuan; Glenn G. Kacprzak; Karl Glazebrook; Lisa J. Kewley; Ivelina Momcheva; Casey J. Papovich; Ryan Quadri; Greg Rudnick; Amélie Saintonge; Lee R. Spitler; Caroline Straatman; Adam Tomczak

doi:10.1088/0004-637X/811/1/28

ZFIRE: galaxy cluster kinematics, Hα star formation rates, and gas phase metallicities of XMM-LSS J02182-05102 at zcl=1.6233

Kim Vy H Tran^*, Themiya Nanayakkara, Tiantian Yuan, Glenn G. Kacprzak, Karl Glazebrook, Lisa J. Kewley, Ivelina Momcheva, Casey J. Papovich, Ryan Quadri, Greg Rudnick, Amélie Saintonge, Lee R. Spitler, Caroline Straatman, Adam Tomczak

^*Corresponding author for this work

Centre in Astronomy, Astrophysics & Astrophotonics

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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 < zspec < 1.635 defined by 33 members of which 20 are at Rproj < 1Mpc. The cluster redshift and velocity dispersion are zcl = 1.6233 ±0.0003 and ±cl = 254 ±50 kms^-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 H α star formation rates (SFR), gas phase metallicities from [N II]/Hα, and stellar masses. We measure an integrated H α SFR of ∼325 M⊙yr^-1 (26 members; Rproj < 2 Mpc) and show that the elevated star formation in the cluster core (Rproj < 0.25Mpc) is driven by the concentration of star-forming members, but the average SFR per Hα-detected galaxy is half that of members at Rproj ∼ 1Mpc. However, we do not detect any environmental imprint when comparing attenuation and gas phase metallicities: the cluster galaxies show similar trends with M ∗as to the field, e.g., more massive galaxies have larger stellar attenuation. IRC 0218s gas phase metallicity-M ∗ 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 (Dt ∼1 Gyr): the MZR for both galaxy clusters are remarkably consistent with each other and virtually identical to several field surveys at z ∼2.

Original language	English
Article number	28
Pages (from-to)	1-16
Number of pages	16
Journal	Astrophysical Journal
Volume	811
Issue number	1
DOIs	https://doi.org/10.1088/0004-637X/811/1/28
Publication status	Published - 20 Sep 2015

Bibliographical note

Copyright 2015 The American Astronomical Society. First published in the Astrophysical journal, 811(1), 28, 2015, published by IOP Publishing. The original publication is available at http://www.doi.org/10.1088/0004-637X/811/1/28. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

Keywords

galaxies: abundances
galaxies: clusters: individual (XMM-LSS J02182-05102)
galaxies: evolution
galaxies: fundamental parameters

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10.1088/0004-637X/811/1/28

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Tran, K. V. H., Nanayakkara, T., Yuan, T., Kacprzak, G. G., Glazebrook, K., Kewley, L. J., Momcheva, I., Papovich, C. J., Quadri, R., Rudnick, G., Saintonge, A., Spitler, L. R., Straatman, C., & Tomczak, A. (2015). ZFIRE: galaxy cluster kinematics, Hα star formation rates, and gas phase metallicities of XMM-LSS J02182-05102 at zcl=1.6233. Astrophysical Journal, 811(1), 1-16. [28]. https://doi.org/10.1088/0004-637X/811/1/28

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title = "ZFIRE: galaxy cluster kinematics, Hα star formation rates, and gas phase metallicities of XMM-LSS J02182-05102 at zcl=1.6233",

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 < zspec < 1.635 defined by 33 members of which 20 are at Rproj < 1Mpc. The cluster redshift and velocity dispersion are zcl = 1.6233 ±0.0003 and ±cl = 254 ±50 kms-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 H α star formation rates (SFR), gas phase metallicities from [N II]/Hα, and stellar masses. We measure an integrated H α SFR of ∼325 M⊙yr-1 (26 members; Rproj < 2 Mpc) and show that the elevated star formation in the cluster core (Rproj < 0.25Mpc) is driven by the concentration of star-forming members, but the average SFR per Hα-detected galaxy is half that of members at Rproj ∼ 1Mpc. However, we do not detect any environmental imprint when comparing attenuation and gas phase metallicities: the cluster galaxies show similar trends with M ∗as to the field, e.g., more massive galaxies have larger stellar attenuation. IRC 0218s gas phase metallicity-M ∗ 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 (Dt ∼1 Gyr): the MZR for both galaxy clusters are remarkably consistent with each other and virtually identical to several field surveys at z ∼2.",

keywords = "galaxies: abundances, galaxies: clusters: individual (XMM-LSS J02182-05102), galaxies: evolution, galaxies: fundamental parameters",

author = "Tran, {Kim Vy H} and Themiya Nanayakkara and Tiantian Yuan and Kacprzak, {Glenn G.} and Karl Glazebrook and Kewley, {Lisa J.} and Ivelina Momcheva and Papovich, {Casey J.} and Ryan Quadri and Greg Rudnick and Am{\'e}lie Saintonge and Spitler, {Lee R.} and Caroline Straatman and Adam Tomczak",

note = "Copyright 2015 The American Astronomical Society. First published in the Astrophysical journal, 811(1), 28, 2015, published by IOP Publishing. The original publication is available at http://www.doi.org/10.1088/0004-637X/811/1/28. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.",

year = "2015",

month = sep,

day = "20",

doi = "10.1088/0004-637X/811/1/28",

language = "English",

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pages = "1--16",

journal = "Astrophysical Journal",

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Tran, KVH, Nanayakkara, T, Yuan, T, Kacprzak, GG, Glazebrook, K, Kewley, LJ, Momcheva, I, Papovich, CJ, Quadri, R, Rudnick, G, Saintonge, A, Spitler, LR, Straatman, C & Tomczak, A 2015, 'ZFIRE: galaxy cluster kinematics, Hα star formation rates, and gas phase metallicities of XMM-LSS J02182-05102 at zcl=1.6233', Astrophysical Journal, vol. 811, no. 1, 28, pp. 1-16. https://doi.org/10.1088/0004-637X/811/1/28

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T2 - galaxy cluster kinematics, Hα star formation rates, and gas phase metallicities of XMM-LSS J02182-05102 at zcl=1.6233

AU - Tran, Kim Vy H

AU - Nanayakkara, Themiya

AU - Yuan, Tiantian

AU - Kacprzak, Glenn G.

AU - Glazebrook, Karl

AU - Kewley, Lisa J.

AU - Momcheva, Ivelina

AU - Papovich, Casey J.

AU - Quadri, Ryan

AU - Rudnick, Greg

AU - Saintonge, Amélie

AU - Spitler, Lee R.

AU - Straatman, Caroline

AU - Tomczak, Adam

N1 - Copyright 2015 The American Astronomical Society. First published in the Astrophysical journal, 811(1), 28, 2015, published by IOP Publishing. The original publication is available at http://www.doi.org/10.1088/0004-637X/811/1/28. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

PY - 2015/9/20

Y1 - 2015/9/20

N2 - 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 < zspec < 1.635 defined by 33 members of which 20 are at Rproj < 1Mpc. The cluster redshift and velocity dispersion are zcl = 1.6233 ±0.0003 and ±cl = 254 ±50 kms-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 H α star formation rates (SFR), gas phase metallicities from [N II]/Hα, and stellar masses. We measure an integrated H α SFR of ∼325 M⊙yr-1 (26 members; Rproj < 2 Mpc) and show that the elevated star formation in the cluster core (Rproj < 0.25Mpc) is driven by the concentration of star-forming members, but the average SFR per Hα-detected galaxy is half that of members at Rproj ∼ 1Mpc. However, we do not detect any environmental imprint when comparing attenuation and gas phase metallicities: the cluster galaxies show similar trends with M ∗as to the field, e.g., more massive galaxies have larger stellar attenuation. IRC 0218s gas phase metallicity-M ∗ 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 (Dt ∼1 Gyr): the MZR for both galaxy clusters are remarkably consistent with each other and virtually identical to several field surveys at z ∼2.

AB - 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 < zspec < 1.635 defined by 33 members of which 20 are at Rproj < 1Mpc. The cluster redshift and velocity dispersion are zcl = 1.6233 ±0.0003 and ±cl = 254 ±50 kms-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 H α star formation rates (SFR), gas phase metallicities from [N II]/Hα, and stellar masses. We measure an integrated H α SFR of ∼325 M⊙yr-1 (26 members; Rproj < 2 Mpc) and show that the elevated star formation in the cluster core (Rproj < 0.25Mpc) is driven by the concentration of star-forming members, but the average SFR per Hα-detected galaxy is half that of members at Rproj ∼ 1Mpc. However, we do not detect any environmental imprint when comparing attenuation and gas phase metallicities: the cluster galaxies show similar trends with M ∗as to the field, e.g., more massive galaxies have larger stellar attenuation. IRC 0218s gas phase metallicity-M ∗ 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 (Dt ∼1 Gyr): the MZR for both galaxy clusters are remarkably consistent with each other and virtually identical to several field surveys at z ∼2.

KW - galaxies: abundances

KW - galaxies: clusters: individual (XMM-LSS J02182-05102)

KW - galaxies: evolution

KW - galaxies: fundamental parameters

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U2 - 10.1088/0004-637X/811/1/28

DO - 10.1088/0004-637X/811/1/28

M3 - Article

VL - 811

SP - 1

EP - 16

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

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ER -

ZFIRE: galaxy cluster kinematics, Hα star formation rates, and gas phase metallicities of XMM-LSS J02182-05102 at zcl=1.6233

Abstract

Bibliographical note

Keywords

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