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Galaxy Zoo: the interplay of quenching mechanisms in the group environment

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Galaxy Zoo : the interplay of quenching mechanisms in the group environment. / Smethurst, R. J.; Lintott, C. J.; Bamford, S. P.; Hart, R. E.; Kruk, S. J.; Masters, K. L.; Nichol, R. C.; Simmons, B. D.

In: Monthly Notices of the Royal Astronomical Society, Vol. 469, No. 3, 11.08.2017, p. 3670-3687.

Research output: Contribution to journalJournal articlepeer-review

Harvard

Smethurst, RJ, Lintott, CJ, Bamford, SP, Hart, RE, Kruk, SJ, Masters, KL, Nichol, RC & Simmons, BD 2017, 'Galaxy Zoo: the interplay of quenching mechanisms in the group environment', Monthly Notices of the Royal Astronomical Society, vol. 469, no. 3, pp. 3670-3687. https://doi.org/10.1093/mnras/stx973

APA

Smethurst, R. J., Lintott, C. J., Bamford, S. P., Hart, R. E., Kruk, S. J., Masters, K. L., Nichol, R. C., & Simmons, B. D. (2017). Galaxy Zoo: the interplay of quenching mechanisms in the group environment. Monthly Notices of the Royal Astronomical Society, 469(3), 3670-3687. https://doi.org/10.1093/mnras/stx973

Vancouver

Smethurst RJ, Lintott CJ, Bamford SP, Hart RE, Kruk SJ, Masters KL et al. Galaxy Zoo: the interplay of quenching mechanisms in the group environment. Monthly Notices of the Royal Astronomical Society. 2017 Aug 11;469(3):3670-3687. https://doi.org/10.1093/mnras/stx973

Author

Smethurst, R. J. ; Lintott, C. J. ; Bamford, S. P. ; Hart, R. E. ; Kruk, S. J. ; Masters, K. L. ; Nichol, R. C. ; Simmons, B. D. / Galaxy Zoo : the interplay of quenching mechanisms in the group environment. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 469, No. 3. pp. 3670-3687.

Bibtex

@article{d941c2a0c145412fb17ab48a73901f1e,
title = "Galaxy Zoo: the interplay of quenching mechanisms in the group environment",
abstract = "Does the environment of a galaxy directly influence the quenching history of a galaxy? Here, we investigate the detailed morphological structures and star formation histories of a sample of SDSS group galaxies with both classifications from Galaxy Zoo 2 and near ultra-violet (NUV) detections in GALEX. We use the optical and NUV colours to infer the quenching time and rate describing a simple exponentially declining star formation history for each galaxy, along with a control sample of field galaxies. We find that the time since quenching and the rate of quenching do not correlate with the relative velocity of a satellite but are correlated with the group potential. This quenching occurs within an average quenching time-scale of ∼ 2.5 Gyr from star forming to complete quiescence, during an average infall time (from ∼10R200 to 0.01R200) of ∼ 2.6 Gyr. Our results suggest that the environment does play a direct role in galaxy quenching through quenching mechanisms that are correlated with the group potential, such as harassment, interactions or starvation. Environmental quenching mechanisms that are correlated with satellite velocity, such as ram-pressure stripping, are not the main cause of quenching in the group environment. We find that no single mechanism dominates over another, except in the most extreme environments or masses. Instead, an interplay of mergers, mass and morphological quenching and environment-driven quenching mechanisms dependent on the group potential drive galaxy evolution in groups.",
author = "Smethurst, {R. J.} and Lintott, {C. J.} and Bamford, {S. P.} and Hart, {R. E.} and Kruk, {S. J.} and Masters, {K. L.} and Nichol, {R. C.} and Simmons, {B. D.}",
year = "2017",
month = aug,
day = "11",
doi = "10.1093/mnras/stx973",
language = "English",
volume = "469",
pages = "3670--3687",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "OXFORD UNIV PRESS",
number = "3",

}

RIS

TY - JOUR

T1 - Galaxy Zoo

T2 - the interplay of quenching mechanisms in the group environment

AU - Smethurst, R. J.

AU - Lintott, C. J.

AU - Bamford, S. P.

AU - Hart, R. E.

AU - Kruk, S. J.

AU - Masters, K. L.

AU - Nichol, R. C.

AU - Simmons, B. D.

PY - 2017/8/11

Y1 - 2017/8/11

N2 - Does the environment of a galaxy directly influence the quenching history of a galaxy? Here, we investigate the detailed morphological structures and star formation histories of a sample of SDSS group galaxies with both classifications from Galaxy Zoo 2 and near ultra-violet (NUV) detections in GALEX. We use the optical and NUV colours to infer the quenching time and rate describing a simple exponentially declining star formation history for each galaxy, along with a control sample of field galaxies. We find that the time since quenching and the rate of quenching do not correlate with the relative velocity of a satellite but are correlated with the group potential. This quenching occurs within an average quenching time-scale of ∼ 2.5 Gyr from star forming to complete quiescence, during an average infall time (from ∼10R200 to 0.01R200) of ∼ 2.6 Gyr. Our results suggest that the environment does play a direct role in galaxy quenching through quenching mechanisms that are correlated with the group potential, such as harassment, interactions or starvation. Environmental quenching mechanisms that are correlated with satellite velocity, such as ram-pressure stripping, are not the main cause of quenching in the group environment. We find that no single mechanism dominates over another, except in the most extreme environments or masses. Instead, an interplay of mergers, mass and morphological quenching and environment-driven quenching mechanisms dependent on the group potential drive galaxy evolution in groups.

AB - Does the environment of a galaxy directly influence the quenching history of a galaxy? Here, we investigate the detailed morphological structures and star formation histories of a sample of SDSS group galaxies with both classifications from Galaxy Zoo 2 and near ultra-violet (NUV) detections in GALEX. We use the optical and NUV colours to infer the quenching time and rate describing a simple exponentially declining star formation history for each galaxy, along with a control sample of field galaxies. We find that the time since quenching and the rate of quenching do not correlate with the relative velocity of a satellite but are correlated with the group potential. This quenching occurs within an average quenching time-scale of ∼ 2.5 Gyr from star forming to complete quiescence, during an average infall time (from ∼10R200 to 0.01R200) of ∼ 2.6 Gyr. Our results suggest that the environment does play a direct role in galaxy quenching through quenching mechanisms that are correlated with the group potential, such as harassment, interactions or starvation. Environmental quenching mechanisms that are correlated with satellite velocity, such as ram-pressure stripping, are not the main cause of quenching in the group environment. We find that no single mechanism dominates over another, except in the most extreme environments or masses. Instead, an interplay of mergers, mass and morphological quenching and environment-driven quenching mechanisms dependent on the group potential drive galaxy evolution in groups.

U2 - 10.1093/mnras/stx973

DO - 10.1093/mnras/stx973

M3 - Journal article

VL - 469

SP - 3670

EP - 3687

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -