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Galaxy Zoo CEERS: Bar Fractions Up to <i>z</i> ∼ 4.0

Research output: Contribution to Journal/Magazine › Journal article › peer-review

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Galaxy Zoo CEERS: Bar Fractions Up to <i>z</i> ∼ 4.0. / Géron, Tobias; Smethurst, R. J.; Dickinson, Hugh et al.
In: The Astrophysical Journal, Vol. 987, No. 1, 74, 01.07.2025.

Research output: Contribution to Journal/Magazine › Journal article › peer-review

Harvard

Géron, T, Smethurst, RJ, Dickinson, H, Fortson, LF, Garland, IL, Kruk, S, Lintott, C, Makechemu, JS, Mantha, KB, Masters, KL, O’Ryan, D, Roberts, H, Simmons, BD, Walmsley, M, Calabrò, A, Chiba, R, Costantin, L, Drout, MR, Fragkoudi, F, Guo, Y, Holwerda, BW, Jogee, S, Koekemoer, AM, Lucas, RA & Pacucci, F 2025, 'Galaxy Zoo CEERS: Bar Fractions Up to <i>z</i> ∼ 4.0', The Astrophysical Journal, vol. 987, no. 1, 74. https://doi.org/10.3847/1538-4357/add7d0

APA

Géron, T., Smethurst, R. J., Dickinson, H., Fortson, L. F., Garland, I. L., Kruk, S., Lintott, C., Makechemu, J. S., Mantha, K. B., Masters, K. L., O’Ryan, D., Roberts, H., Simmons, B. D., Walmsley, M., Calabrò, A., Chiba, R., Costantin, L., Drout, M. R., Fragkoudi, F., ... Pacucci, F. (2025). Galaxy Zoo CEERS: Bar Fractions Up to <i>z</i> ∼ 4.0. The Astrophysical Journal, 987(1), Article 74. https://doi.org/10.3847/1538-4357/add7d0

Vancouver

Géron T, Smethurst RJ, Dickinson H, Fortson LF, Garland IL, Kruk S et al. Galaxy Zoo CEERS: Bar Fractions Up to <i>z</i> ∼ 4.0. The Astrophysical Journal. 2025 Jul 1;987(1):74. Epub 2025 Jun 30. doi: 10.3847/1538-4357/add7d0

Author

Géron, Tobias ; Smethurst, R. J. ; Dickinson, Hugh et al. / Galaxy Zoo CEERS : Bar Fractions Up to <i>z</i> ∼ 4.0. In: The Astrophysical Journal. 2025 ; Vol. 987, No. 1.

Bibtex

@article{8450d32a4bcb49db913ef5b740b40d11,
title = "Galaxy Zoo CEERS: Bar Fractions Up to z ∼ 4.0",
abstract = "We study the evolution of the bar fraction in disk galaxies between 0.5 < z < 4.0 using multiband colored images from JWST Cosmic Evolution Early Release Science Survey (CEERS). These images were classified by citizen scientists in a new phase of the Galaxy Zoo (GZ) project called GZ CEERS. Citizen scientists were asked whether a strong or weak bar was visible in the host galaxy. After considering multiple corrections for observational biases, we find that the bar fraction decreases with redshift in our volume-limited sample (n = 398); from 2 5 − 4 + 6 % at 0.5 < z < 1.0 to 3 − 1 + 6 % at 3.0 < z < 4.0. However, we argue it is appropriate to interpret these fractions as lower limits. Disentangling real changes in the bar fraction from detection biases remains challenging. Nevertheless, we find a significant number of bars up to z = 2.5. This implies that disks are dynamically cool or baryon dominated, enabling them to host bars. This also suggests that bar-driven secular evolution likely plays an important role at higher redshifts. When we distinguish between strong and weak bars, we find that the weak bar fraction decreases with increasing redshift. In contrast, the strong bar fraction is constant between 0.5 < z < 2.5. This implies that the strong bars found in this work are robust long-lived structures, unless the rate of bar destruction is similar to the rate of bar formation. Finally, our results are consistent with disk instabilities being the dominant mode of bar formation at lower redshifts, while bar formation through interactions and mergers is more common at higher redshifts.",
author = "Tobias G{\'e}ron and Smethurst, {R. J.} and Hugh Dickinson and Fortson, {L. F.} and Garland, {Izzy L.} and Sandor Kruk and Chris Lintott and Makechemu, {Jason Shingirai} and Mantha, {Kameswara Bharadwaj} and Masters, {Karen L.} and David O{\textquoteright}Ryan and Hayley Roberts and Simmons, {B. D.} and Mike Walmsley and Antonello Calabr{\`o} and Rimpei Chiba and Luca Costantin and Drout, {Maria R.} and Francesca Fragkoudi and Yuchen Guo and Holwerda, {B. W.} and Shardha Jogee and Koekemoer, {Anton M.} and Lucas, {Ray A.} and Fabio Pacucci",
year = "2025",
month = jul,
day = "1",
doi = "10.3847/1538-4357/add7d0",
language = "English",
volume = "987",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing",
number = "1",

}

RIS

TY - JOUR

T1 - Galaxy Zoo CEERS

T2 - Bar Fractions Up to z ∼ 4.0

AU - Géron, Tobias

AU - Smethurst, R. J.

AU - Dickinson, Hugh

AU - Fortson, L. F.

AU - Garland, Izzy L.

AU - Kruk, Sandor

AU - Lintott, Chris

AU - Makechemu, Jason Shingirai

AU - Mantha, Kameswara Bharadwaj

AU - Masters, Karen L.

AU - O’Ryan, David

AU - Roberts, Hayley

AU - Simmons, B. D.

AU - Walmsley, Mike

AU - Calabrò, Antonello

AU - Chiba, Rimpei

AU - Costantin, Luca

AU - Drout, Maria R.

AU - Fragkoudi, Francesca

AU - Guo, Yuchen

AU - Holwerda, B. W.

AU - Jogee, Shardha

AU - Koekemoer, Anton M.

AU - Lucas, Ray A.

AU - Pacucci, Fabio

PY - 2025/7/1

Y1 - 2025/7/1

N2 - We study the evolution of the bar fraction in disk galaxies between 0.5 < z < 4.0 using multiband colored images from JWST Cosmic Evolution Early Release Science Survey (CEERS). These images were classified by citizen scientists in a new phase of the Galaxy Zoo (GZ) project called GZ CEERS. Citizen scientists were asked whether a strong or weak bar was visible in the host galaxy. After considering multiple corrections for observational biases, we find that the bar fraction decreases with redshift in our volume-limited sample (n = 398); from 2 5 − 4 + 6 % at 0.5 < z < 1.0 to 3 − 1 + 6 % at 3.0 < z < 4.0. However, we argue it is appropriate to interpret these fractions as lower limits. Disentangling real changes in the bar fraction from detection biases remains challenging. Nevertheless, we find a significant number of bars up to z = 2.5. This implies that disks are dynamically cool or baryon dominated, enabling them to host bars. This also suggests that bar-driven secular evolution likely plays an important role at higher redshifts. When we distinguish between strong and weak bars, we find that the weak bar fraction decreases with increasing redshift. In contrast, the strong bar fraction is constant between 0.5 < z < 2.5. This implies that the strong bars found in this work are robust long-lived structures, unless the rate of bar destruction is similar to the rate of bar formation. Finally, our results are consistent with disk instabilities being the dominant mode of bar formation at lower redshifts, while bar formation through interactions and mergers is more common at higher redshifts.

AB - We study the evolution of the bar fraction in disk galaxies between 0.5 < z < 4.0 using multiband colored images from JWST Cosmic Evolution Early Release Science Survey (CEERS). These images were classified by citizen scientists in a new phase of the Galaxy Zoo (GZ) project called GZ CEERS. Citizen scientists were asked whether a strong or weak bar was visible in the host galaxy. After considering multiple corrections for observational biases, we find that the bar fraction decreases with redshift in our volume-limited sample (n = 398); from 2 5 − 4 + 6 % at 0.5 < z < 1.0 to 3 − 1 + 6 % at 3.0 < z < 4.0. However, we argue it is appropriate to interpret these fractions as lower limits. Disentangling real changes in the bar fraction from detection biases remains challenging. Nevertheless, we find a significant number of bars up to z = 2.5. This implies that disks are dynamically cool or baryon dominated, enabling them to host bars. This also suggests that bar-driven secular evolution likely plays an important role at higher redshifts. When we distinguish between strong and weak bars, we find that the weak bar fraction decreases with increasing redshift. In contrast, the strong bar fraction is constant between 0.5 < z < 2.5. This implies that the strong bars found in this work are robust long-lived structures, unless the rate of bar destruction is similar to the rate of bar formation. Finally, our results are consistent with disk instabilities being the dominant mode of bar formation at lower redshifts, while bar formation through interactions and mergers is more common at higher redshifts.

U2 - 10.3847/1538-4357/add7d0

DO - 10.3847/1538-4357/add7d0

M3 - Journal article

VL - 987

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 74

ER -