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    Rights statement: This is an author-created, un-copyedited version of an article accepted for publication/published in The Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi: 10.3847/1538-4357/abe5a3.

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Evidence for gas-phase metal deficiency in massive protocluster galaxies at z~2.2

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Evidence for gas-phase metal deficiency in massive protocluster galaxies at z~2.2. / Sattari, Zahra; Mobasher, Bahram; Chartab, Nima; Darvish, Behnam; Shivaei, Irene; Scoville, Nick; Sobral, David.

In: The Astrophysical Journal, Vol. 910, No. 1, 57, 25.03.2021.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

Sattari, Z, Mobasher, B, Chartab, N, Darvish, B, Shivaei, I, Scoville, N & Sobral, D 2021, 'Evidence for gas-phase metal deficiency in massive protocluster galaxies at z~2.2', The Astrophysical Journal, vol. 910, no. 1, 57. https://doi.org/10.3847/1538-4357/abe5a3/meta

APA

Sattari, Z., Mobasher, B., Chartab, N., Darvish, B., Shivaei, I., Scoville, N., & Sobral, D. (2021). Evidence for gas-phase metal deficiency in massive protocluster galaxies at z~2.2. The Astrophysical Journal, 910(1), [57]. https://doi.org/10.3847/1538-4357/abe5a3/meta

Vancouver

Sattari Z, Mobasher B, Chartab N, Darvish B, Shivaei I, Scoville N et al. Evidence for gas-phase metal deficiency in massive protocluster galaxies at z~2.2. The Astrophysical Journal. 2021 Mar 25;910(1). 57. https://doi.org/10.3847/1538-4357/abe5a3/meta

Author

Sattari, Zahra ; Mobasher, Bahram ; Chartab, Nima ; Darvish, Behnam ; Shivaei, Irene ; Scoville, Nick ; Sobral, David. / Evidence for gas-phase metal deficiency in massive protocluster galaxies at z~2.2. In: The Astrophysical Journal. 2021 ; Vol. 910, No. 1.

Bibtex

@article{d89514cdcd574faa89ccecae4150b608,
title = "Evidence for gas-phase metal deficiency in massive protocluster galaxies at z~2.2",
abstract = " We study the mass-metallicity relation for 19 members of a spectroscopically-confirmed protocluster in the COSMOS field at $z=2.2$ (CC2.2), and compare it with that of 24 similarly selected field galaxies at the same redshift. Both samples are $\rm H\alpha$ emitting sources, chosen from the HiZELS narrow-band survey, with metallicities derived from $\rm N2\ (\frac{\rm [NII] \lambda 6584}{\rm H \alpha})$ line ratio. For the mass-matched samples of protocluster and field galaxies, we find that protocluster galaxies with $10^{9.9} \rm M_\odot \leq M_* \leq 10^{10.9} \rm M_\odot$ are metal deficient by $0.10 \pm 0.04$ dex ($2.5\sigma$ significance) compared to their coeval field galaxies. This metal deficiency is absent for low mass galaxies, $\rm M_* <10^{9.9} \rm M_\odot$. Moreover, relying on both SED-derived and $\rm {H\alpha}$ (corrected for dust extinction based on $\rm {M_*}$) SFRs, we find no strong environmental dependence of SFR-$\rm {M_*}$ relation, however, we are not able to rule out the existence of small dependence due to inherent uncertainties in both SFR estimators. The existence of $2.5\sigma$ significant metal deficiency for massive protocluster galaxies favors a model in which funneling of the primordial cold gas through filaments dilutes the metal content of protoclusters at high redshifts ($z \gtrsim 2$). At these redshifts, gas reservoirs in filaments are dense enough to cool down rapidly and fall into the potential well of the protocluster to lower the gas-phase metallicity of galaxies. Moreover, part of this metal deficiency could be originated from galaxy interactions which are more prevalent in dense environments. ",
keywords = "astro-ph.GA",
author = "Zahra Sattari and Bahram Mobasher and Nima Chartab and Behnam Darvish and Irene Shivaei and Nick Scoville and David Sobral",
note = "This is an author-created, un-copyedited version of an article accepted for publication/published in The Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi: 10.3847/1538-4357/abe5a3.",
year = "2021",
month = mar,
day = "25",
doi = "10.3847/1538-4357/abe5a3/meta",
language = "English",
volume = "910",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing",
number = "1",

}

RIS

TY - JOUR

T1 - Evidence for gas-phase metal deficiency in massive protocluster galaxies at z~2.2

AU - Sattari, Zahra

AU - Mobasher, Bahram

AU - Chartab, Nima

AU - Darvish, Behnam

AU - Shivaei, Irene

AU - Scoville, Nick

AU - Sobral, David

N1 - This is an author-created, un-copyedited version of an article accepted for publication/published in The Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi: 10.3847/1538-4357/abe5a3.

PY - 2021/3/25

Y1 - 2021/3/25

N2 - We study the mass-metallicity relation for 19 members of a spectroscopically-confirmed protocluster in the COSMOS field at $z=2.2$ (CC2.2), and compare it with that of 24 similarly selected field galaxies at the same redshift. Both samples are $\rm H\alpha$ emitting sources, chosen from the HiZELS narrow-band survey, with metallicities derived from $\rm N2\ (\frac{\rm [NII] \lambda 6584}{\rm H \alpha})$ line ratio. For the mass-matched samples of protocluster and field galaxies, we find that protocluster galaxies with $10^{9.9} \rm M_\odot \leq M_* \leq 10^{10.9} \rm M_\odot$ are metal deficient by $0.10 \pm 0.04$ dex ($2.5\sigma$ significance) compared to their coeval field galaxies. This metal deficiency is absent for low mass galaxies, $\rm M_* <10^{9.9} \rm M_\odot$. Moreover, relying on both SED-derived and $\rm {H\alpha}$ (corrected for dust extinction based on $\rm {M_*}$) SFRs, we find no strong environmental dependence of SFR-$\rm {M_*}$ relation, however, we are not able to rule out the existence of small dependence due to inherent uncertainties in both SFR estimators. The existence of $2.5\sigma$ significant metal deficiency for massive protocluster galaxies favors a model in which funneling of the primordial cold gas through filaments dilutes the metal content of protoclusters at high redshifts ($z \gtrsim 2$). At these redshifts, gas reservoirs in filaments are dense enough to cool down rapidly and fall into the potential well of the protocluster to lower the gas-phase metallicity of galaxies. Moreover, part of this metal deficiency could be originated from galaxy interactions which are more prevalent in dense environments.

AB - We study the mass-metallicity relation for 19 members of a spectroscopically-confirmed protocluster in the COSMOS field at $z=2.2$ (CC2.2), and compare it with that of 24 similarly selected field galaxies at the same redshift. Both samples are $\rm H\alpha$ emitting sources, chosen from the HiZELS narrow-band survey, with metallicities derived from $\rm N2\ (\frac{\rm [NII] \lambda 6584}{\rm H \alpha})$ line ratio. For the mass-matched samples of protocluster and field galaxies, we find that protocluster galaxies with $10^{9.9} \rm M_\odot \leq M_* \leq 10^{10.9} \rm M_\odot$ are metal deficient by $0.10 \pm 0.04$ dex ($2.5\sigma$ significance) compared to their coeval field galaxies. This metal deficiency is absent for low mass galaxies, $\rm M_* <10^{9.9} \rm M_\odot$. Moreover, relying on both SED-derived and $\rm {H\alpha}$ (corrected for dust extinction based on $\rm {M_*}$) SFRs, we find no strong environmental dependence of SFR-$\rm {M_*}$ relation, however, we are not able to rule out the existence of small dependence due to inherent uncertainties in both SFR estimators. The existence of $2.5\sigma$ significant metal deficiency for massive protocluster galaxies favors a model in which funneling of the primordial cold gas through filaments dilutes the metal content of protoclusters at high redshifts ($z \gtrsim 2$). At these redshifts, gas reservoirs in filaments are dense enough to cool down rapidly and fall into the potential well of the protocluster to lower the gas-phase metallicity of galaxies. Moreover, part of this metal deficiency could be originated from galaxy interactions which are more prevalent in dense environments.

KW - astro-ph.GA

U2 - 10.3847/1538-4357/abe5a3/meta

DO - 10.3847/1538-4357/abe5a3/meta

M3 - Journal article

VL - 910

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 57

ER -