pith. sign in

arxiv: 2606.23792 · v1 · pith:Q3FSRXHPnew · submitted 2026-06-22 · 🌌 astro-ph.GA

Discovery of a Barred-Spiral Galaxy at z_(spec) = 3.16 I: Bar Identification and Properties

Daniel Ivanov , Mauro Giavalisco , Yingjie Cheng , Yuchen Guo , Luca Costantin , Elena D'Onghia , John R. Weaver , Shardha Jogee
show 1 more author
Katherine E. Whitaker
This is my paper

Pith reviewed 2026-06-26 08:00 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords barred spiral galaxyhigh-redshift galaxiesJWST imaginggalactic barsdisk galaxy evolutionCOSMOS-74706z=3.16secular evolution
0
0 comments X

The pith

A barred spiral galaxy at spectroscopic redshift 3.159 shows rotationally supported disks were already in place within 2 Gyr after the Big Bang.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper reports the discovery of COSMOS-74706, a barred spiral galaxy at z_spec = 3.159. JWST/NIRCam imaging reveals a disk-like morphology with spiral arms and an elongated central feature. Three methods confirm the bar: residuals after Sersic fitting show a linear structure, isophotal ellipse fitting matches bar signatures in ellipticity and position angle, and Fourier decomposition yields a strong central bisymmetric mode. Archival Keck/MOSDEF spectroscopy of a blue clump overlapping the galaxy provides a robust redshift, with photometry indicating the clump shares the same redshift as the main body.

Core claim

The central claim is the identification of COSMOS-74706 as an unlensed barred spiral at z_spec=3.159. The bar is established through visual inspection of Sersic-profile residuals revealing a linear feature, isophotal ellipse-fitting displaying the characteristic ellipticity and position-angle profiles of a bar, and Fourier decomposition producing a central bisymmetric mode above the strength threshold calibrated on lower-redshift barred spirals. The Keck spectrum secures the redshift, placing the galaxy at z>3 and supporting the presence of galaxies with rotationally supported disks and disk-halo properties conducive to bar formation within 2 Gyr after the Big Bang.

What carries the argument

Bar identification in COSMOS-74706 via three independent techniques on JWST/NIRCam data: Sersic residual analysis for linear structure, isophotal ellipse-fitting for ellipticity and position angle signatures, and Fourier decomposition for bisymmetric mode strength, combined with Keck spectroscopic redshift confirmation.

If this is right

  • Rotationally supported disks with properties allowing bar formation existed by z=3.16.
  • Secular evolution processes driven by bars began within the first 2 Gyr of cosmic time.
  • Disk-halo configurations conducive to bar instabilities were already assembled at early epochs.
  • Bar formation is possible in galaxies at redshifts previously thought too early for mature disks.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Models of galaxy disk assembly may need to incorporate bar formation as an early process rather than a late-time feature.
  • Targeted JWST follow-up on other high-redshift candidates could establish how common such bars are at z>3.
  • This case provides a concrete benchmark for simulations testing the conditions required for bars in young galaxies.

Load-bearing premise

The elongated central feature is a stellar bar and not a merger remnant or projection effect, and the Keck spectrum of the blue clump applies to the main galaxy body.

What would settle it

Higher-resolution imaging or additional spectroscopy demonstrating that the central feature is a tidal tail or that the main body lies at a different redshift would falsify the barred-spiral identification at z=3.16.

Figures

Figures reproduced from arXiv: 2606.23792 by Daniel Ivanov, Elena D'Onghia, John R. Weaver, Katherine E. Whitaker, Luca Costantin, Mauro Giavalisco, Shardha Jogee, Yingjie Cheng, Yuchen Guo.

Figure 1
Figure 1. Figure 1: The panels are images of COSMOS-74706 which visually highlight the prominent spiral arms and prospective central bar structure. Each picture covers 2.6 arcseconds, corresponding to a physical scale of approximately 20 kpc along each side. Left panel: A composition of COSMOS-74706 in the F200W, F277W, and F356W filters shows the spiral arms and a pronounced bulge as well as the blue northern element directl… view at source ↗
Figure 2
Figure 2. Figure 2: Best-fit SEDs of COSMOS-74706 are shown at left, including fits to the entire galaxy (black), with the blue northern element masked (green), and on the bulge region only (red). The gray curves at the bottom depict the transmission of the available filters. Histograms on the right side depict the corresponding redshift probability distributions p(z) with the solid black vertical lines depicting the best fit… view at source ↗
Figure 3
Figure 3. Figure 3: GALFIT decompositions of COSMOS-74706 found by MCMC exploration in three different JWST/NIRCam filters as indicated on the left. The columns display from left to right (1) the science mosaic image, (2) the same image but with the northern element masked, (3) the full two-component GALFIT model of the light profile, (4) the inner component of the model, (5) the outer component, and (6) the model residual wi… view at source ↗
Figure 4
Figure 4. Figure 4: Upper panel: The sum of the best-fit 2-component S´ersic light profile models for all three filters subtracted from the sum of the three images at the 3σ mask cutoff level. A bar-like structure can be seen connecting the residuals of the spiral arms. Lower panel: As upper panel but with the inner light profiles added back in with a different stretch to highlight the elongation without saturating the image.… view at source ↗
Figure 5
Figure 5. Figure 5: The three panels depict histograms of the distribution of differences between the position angle of the disk and bar components (θdisk − θbar) in the posterior of the two-component S´ersic models of COSMOS-74706. The top part of each panel shows a zoomed-in view of the distribution. The circular insets depict the position angles themselves with the inner solid lines representing the orientation of the prof… view at source ↗
Figure 6
Figure 6. Figure 6: shows the results of the Isophotal and Fourier analysis. The two modes collectively display the most positive bar identifications in the F200W and F277W fil￾ters where the bar is most easily visually ascertainable. In fact the Fourier analysis shows positive bar identi￾fications across all mask noise-cutoffs in the F150W, F200W, F277W, F356W, and F410M filters as well as one positive identification at the … view at source ↗
Figure 7
Figure 7. Figure 7: The panels display the results of the isophotal analysis of COSMOS-74706 in six JWST/NIRCam filters as labeled. The various mask noise-level cutoffs are overlaid on top of one another in each panel, showing from top to bottom the surface brightness, ellipticity, and position angle of the isophotes moving radially outward. A PA of 0◦ corresponds to an ellipse whose semi-major axis lies along the East-West a… view at source ↗
Figure 8
Figure 8. Figure 8: Fourier amplitudes |A(p, m)| from the decom￾position of COSMOS-74706 into logarithmic spirals. Each panel shows a different multiplicity mode m as a function of the pitch angle parameter p. The different line styles rep￾resent various JWST/NIRCam filters with the 2.5σ mask. Corresponding bar strength parameters BM are listed in the legend for each filter and are commensurate with each fil￾ter’s strength in… view at source ↗
Figure 9
Figure 9. Figure 9: A log-polar unwrapping of COSMOS-74706 across filters shows the surface brightness plotted by az￾imuthal angle θ and radius ln r. The tapered inner region is not depicted. The apparent decreasing surface brightness towards longer filters is a consequence of increased contrast between the surface brightness at the center and outer re￾gions of the galaxy. 2025, Ivanov et al. in prep). Given the suggestion of… view at source ↗
Figure 10
Figure 10. Figure 10: Radial Fourier decomposition of the m = 2 mode for COSMOS-74706 in F150W, F200W, F277W, and F356W. The gray shaded band demarcates the bar region and the dotted line on the bottom panel indicates the disk PA. Top: normalized m = 2 amplitude A2 as a function of galactocentric radius. Bottom: m = 2 phase ϕ2(R) expressed as a position angle measured east of north. Faded markers indicate radii where A2 falls … view at source ↗
Figure 11
Figure 11. Figure 11: The BM computed for different values of the outermost radius included in the Fourier decomposition of COSMOS-74706 using the 2.5σ masked images in each of three filters. Radii for which BM was not computed due to the absence of a central Gaussian are excluded. The identi￾fied end of the bar region is the same as in [PITH_FULL_IMAGE:figures/full_fig_p019_11.png] view at source ↗
read the original abstract

The formation of stellar bars is an important milestone in the secular evolution of spiral galaxies, which typically indicates the presence of a massive rotationally supported disk. Determining when these structures first appeared in the early universe is crucial to constraining the timeline of galactic disk assembly. Here, we report the discovery of COSMOS-74706, a barred spiral galaxy at $z_{spec} = 3.159$. Imaging of COSMOS-74706 with JWST/NIRCam indicates a disk-like morphology and spiral structure with an elongated central feature aligned between the spiral arms, most conspicuously visible in the F200W, F277W, and F356W filters. Three independent methods all support the presence of a bar: visual inspection of residuals from S\'ersic-profile fitting shows a linear structure, isophotal ellipse-fitting displays characteristic profiles of ellipticity and position angle consistent with a bar signature, and Fourier decomposition of the galaxy produces a central bisymmetric mode above a threshold strength calibrated to $z=1-3$ barred spirals. Leveraging archival Keck/MOSDEF spectroscopy overlapping with a blue clump on the edge of the galaxy, a robust redshift is inferred, with photometric constraints indicating that this structure lies at the same redshift as the main spiral. This spectroscopic evidence, placing an unlensed barred spiral at $z>3$ supports the idea that galaxies with rotationally supported disks and disk-halo properties that are conducive to bar formation were already in place within 2 Gyr after the Big Bang.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper reports the discovery of COSMOS-74706, an unlensed barred spiral galaxy at z_spec=3.159. JWST/NIRCam imaging shows a disk-like morphology with spiral arms and an elongated central feature; three methods (Sersic residual inspection, isophotal ellipse fitting, and Fourier decomposition with a bisymmetric mode above a z=1-3 calibrated threshold) support bar identification. Archival Keck/MOSDEF spectroscopy of an offset blue clump yields the redshift, with photometric constraints invoked to associate the clump and main body at the same z. This is presented as evidence that rotationally supported disks conducive to bar formation existed within 2 Gyr after the Big Bang.

Significance. If the redshift association and bar identification are robust, the result would provide direct evidence for early bar formation at z>3, constraining the timeline of disk assembly and secular evolution in the early universe. The use of multiple independent bar-identification methods and archival spectroscopy adds value, though the claim's impact hinges on confirming the main galaxy's redshift.

major comments (2)
  1. [redshift determination] The spectroscopic redshift z_spec=3.159 is obtained exclusively from a blue clump at the galaxy edge rather than the main stellar body (see abstract and redshift paragraph). The association relies on photometric constraints, but no quantitative details (e.g., photo-z probability distributions, chi-squared values, or chance-alignment probability) are provided to demonstrate that a different redshift for the clump is ruled out at high . This association is load-bearing for the z>3 claim and the timeline argument.
  2. [bar identification methods] The Fourier decomposition method invokes a bisymmetric mode strength threshold calibrated on z=1-3 barred spirals (abstract), but no explicit value, uncertainty, or test of applicability at z=3.16 (where surface brightness dimming and resolution effects differ) is reported. Without this, it is unclear whether the central mode detection is robust or could be affected by noise or projection.
minor comments (2)
  1. [abstract] The abstract states that three methods support the bar but provides no quantitative thresholds, error bars, or comparison metrics (e.g., ellipticity peak value or Fourier amplitude). Adding these would improve clarity.
  2. The claim of an 'unlensed' galaxy should include a brief justification or reference to lensing models for the COSMOS field to rule out significant magnification.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review. We address the two major comments point by point below. Both concerns identify areas where the current manuscript lacks sufficient quantitative detail; we will incorporate the requested information in the revised version.

read point-by-point responses

  1. Referee: The spectroscopic redshift z_spec=3.159 is obtained exclusively from a blue clump at the galaxy edge rather than the main stellar body (see abstract and redshift paragraph). The association relies on photometric constraints, but no quantitative details (e.g., photo-z probability distributions, chi-squared values, or chance-alignment probability) are provided to demonstrate that a different redshift for the clump is ruled out at high confidence. This association is load-bearing for the z>3 claim and the timeline argument.

    Authors: We agree that the manuscript does not currently supply the quantitative photometric details needed to rigorously support the redshift association. In the revised version we will add the photometric redshift probability distributions for both the main galaxy and the offset blue clump, the associated chi-squared values, and an estimate of the chance-alignment probability. These additions will directly address the load-bearing nature of the association. revision: yes

  2. Referee: The Fourier decomposition method invokes a bisymmetric mode strength threshold calibrated on z=1-3 barred spirals (abstract), but no explicit value, uncertainty, or test of applicability at z=3.16 (where surface brightness dimming and resolution effects differ) is reported. Without this, it is unclear whether the central mode detection is robust or could be affected by noise or projection.

    Authors: The referee is correct that the explicit numerical value of the bisymmetric Fourier mode amplitude, its uncertainty, and any discussion of the calibration's applicability at z=3.16 are absent from the present text. We will revise the manuscript to report the measured mode strength with uncertainty, state its relation to the z=1-3 threshold, and include a short discussion of possible surface-brightness-dimming and resolution effects. The bar identification rests on three independent methods, so the Fourier result will be presented in that context. revision: yes

Circularity Check

0 steps flagged

No circularity: direct observational identification

full rationale

The paper reports an observational discovery using JWST/NIRCam imaging for morphology (Sersic residuals, isophotal fitting, Fourier modes) and archival Keck/MOSDEF spectroscopy for redshift, with photometric constraints to associate the blue clump spectrum with the main galaxy. No mathematical derivation chain, fitted parameters renamed as predictions, or self-citation load-bearing steps exist. The bar threshold is calibrated externally to z=1-3 samples, and the redshift association is an inference from photometry rather than a self-referential reduction. This is a standard observational result with no internal loop.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The work relies on standard cosmological distance conversions and a bar-strength threshold calibrated on lower-redshift samples; no new entities are introduced.

free parameters (1)
  • Fourier bisymmetric mode threshold
    Calibrated to z=1-3 barred spirals to decide bar presence
axioms (1)
  • standard math Standard flat Lambda-CDM cosmology for converting redshift to cosmic time
    Invoked to state the galaxy existed within 2 Gyr after the Big Bang

pith-pipeline@v0.9.1-grok · 5847 in / 1166 out tokens · 31149 ms · 2026-06-26T08:00:27.795065+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

95 extracted references · 78 canonical work pages · 3 internal anchors

  1. [1]

    Gadotti, D

    A. Gadotti, D. 2009, in Chaos in Astronomy, ed. G. Contopoulos & P. A. Patsis (Berlin, Heidelberg: Springer Berlin Heidelberg), 159–172

    2009

  2. [2]

    Aguerri, J. A. L., M´ endez-Abreu, J., & Corsini, E. M. 2009, Astronomy & Astrophysics, 495, 491–504, doi: 10.1051/0004-6361:200810931

    work page doi:10.1051/0004-6361:200810931 2009

  3. [3]

    W., et al

    Amvrosiadis, A., Lange, S., Nightingale, J. W., et al. 2025, Monthly Notices of the Royal Astronomical Society, 537, 1163, doi: 10.1093/mnras/staf048 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sip˝ ocz, B. M., et al. 2018, AJ, 156, 123,...

    work page doi:10.1093/mnras/staf048 2025

  4. [4]

    , keywords =

    Athanassoula, E. 1992, MNRAS, 259, 345, doi: 10.1093/mnras/259.2.345

    work page doi:10.1093/mnras/259.2.345 1992

  5. [5]

    , keywords =

    Athanassoula, E. 2003, Monthly Notices of the Royal Astronomical Society, 341, 1179–1198, doi: 10.1046/j.1365-8711.2003.06473.x —. 2013, Bars and secular evolution in disk galaxies: Theoretical input, ed. J. Falc´ on-Barroso & J. H. Knapen, Canary Islands Winter School of Astrophysics (Cambridge University Press), 305–352

    work page doi:10.1046/j.1365-8711.2003.06473.x 2003

  6. [6]

    Athanassoula, E., Machado, R. E. G., & Rodionov, S. A. 2013, Monthly Notices of the Royal Astronomical Society, 429, 1949, doi: 10.1093/mnras/sts452 22Ivanov et al

    work page doi:10.1093/mnras/sts452 2013

  7. [7]

    2002, MNRAS, 334, 523, doi: 10.1046/j.1365-8711.2002.05478.x

    Athanassoula, E., & Misiriotis, A. 2002, Monthly Notices of the Royal Astronomical Society, 330, 35–52, doi: 10.1046/j.1365-8711.2002.05028.x

    work page doi:10.1046/j.1365-8711.2002.05028.x 2002

  8. [8]

    , keywords =

    Bamford, S. P., Nichol, R. C., Baldry, I. K., et al. 2009, Monthly Notices of the Royal Astronomical Society, 393, 1324–1352, doi: 10.1111/j.1365-2966.2008.14252.x

    work page doi:10.1111/j.1365-2966.2008.14252.x 2009

  9. [9]

    , keywords =

    Barazza, F. D., Jogee, S., & Marinova, I. 2008, ApJ, 675, 1194, doi: 10.1086/526510

    work page doi:10.1086/526510 2008

  10. [10]

    2023, ApJ, 953, 173, doi: 10.3847/1538-4357/ace2b9

    Beane, A., Hernquist, L., D’Onghia, E., et al. 2023, ApJ, 953, 173, doi: 10.3847/1538-4357/ace2b9

    work page doi:10.3847/1538-4357/ace2b9 2023

  11. [11]

    2022, ApJ, 934, 52, doi: 10.3847/1538-4357/ac779b

    Bi, D., Shlosman, I., & Romano-D´ ıaz, E. 2022, ApJ, 934, 52, doi: 10.3847/1538-4357/ac779b

    work page doi:10.3847/1538-4357/ac779b 2022

  12. [12]

    2024, Turbulent gas-rich disks at high redshift: bars & bulges in a radial shear flow

    Federrath, C. 2024, Turbulent gas-rich disks at high redshift: bars & bulges in a radial shear flow. https://arxiv.org/abs/2402.06060

    arXiv 2024

  13. [13]

    2023, The Astrophysical Journal, 947, 80, doi: 10.3847/1538-4357/acc469

    Freeman, K. 2023, The Astrophysical Journal, 947, 80, doi: 10.3847/1538-4357/acc469

    work page doi:10.3847/1538-4357/acc469 2023

  14. [14]

    L., Buta, R., Knapen, J

    Block, D. L., Buta, R., Knapen, J. H., et al. 2004, The Astronomical Journal, 128, 183–201, doi: 10.1086/421362

    work page doi:10.1086/421362 2004

  15. [15]

    , keywords =

    Bournaud, F., Combes, F., & Semelin, B. 2005, MNRAS, 364, L18, doi: 10.1111/j.1745-3933.2005.00096.x

    work page doi:10.1111/j.1745-3933.2005.00096.x 2005

  16. [16]

    2002, A&A, 392, 83, doi: 10.1051/0004-6361:20020920

    Bournaud, F., & Combes, F. 2002, A&A, 392, 83, doi: 10.1051/0004-6361:20020920

    work page doi:10.1051/0004-6361:20020920 2002

  17. [17]

    2024, astropy/photutils: 2.0.2, 2.0.2, Zenodo, doi: 10.5281/zenodo.13989456

    Bradley, L., Sip˝ ocz, B., Robitaille, T., et al. 2024, astropy/photutils: 2.0.2, 2.0.2, Zenodo, doi: 10.5281/zenodo.13989456

    work page doi:10.5281/zenodo.13989456 2024

  18. [18]

    2019, Grizli: Grism redshift and line analysis software, Astrophysics Source Code Library, record ascl:1905.001

    Brammer, G. 2019, Grizli: Grism redshift and line analysis software, Astrophysics Source Code Library, record ascl:1905.001. http://ascl.net/1905.001

    2019

  19. [19]

    B., van Dokkum, P

    Brammer, G. B., van Dokkum, P. G., & Coppi, P. 2008, ApJ, 686, 1503, doi: 10.1086/591786

    work page internal anchor Pith review doi:10.1086/591786 2008

  20. [20]

    B., van Dokkum, P

    Brammer, G. B., van Dokkum, P. G., Franx, M., et al. 2012, ApJS, 200, 13, doi: 10.1088/0067-0049/200/2/13

    work page doi:10.1088/0067-0049/200/2/13 2012

  21. [21]

    J., Knapen, J

    Buta, R. J., Knapen, J. H., Elmegreen, B. G., et al. 2009, The Astronomical Journal, 137, 4487–4516, doi: 10.1088/0004-6256/137/5/4487

    work page doi:10.1088/0004-6256/137/5/4487 2009

  22. [22]

    L., & Kawata, D

    Carles, C., Martel, H., Ellison, S. L., & Kawata, D. 2016, MNRAS, 463, 1074, doi: 10.1093/mnras/stw2056

    work page doi:10.1093/mnras/stw2056 2016

  23. [23]

    , keywords =

    Casey, C. M., Kartaltepe, J. S., Drakos, N. E., et al. 2023, ApJ, 954, 31, doi: 10.3847/1538-4357/acc2bc

    work page doi:10.3847/1538-4357/acc2bc 2023

  24. [24]

    Conselice, C. J. 2014, Annual Review of Astronomy and Astrophysics, 52, 291–337, doi: 10.1146/annurev-astro-081913-040037

    work page doi:10.1146/annurev-astro-081913-040037 2014

  25. [25]

    1988, A&AS, 76, 365

    Considere, S., & Athanassoula, E. 1988, A&AS, 76, 365

    1988

  26. [26]

    Conte, Z. A. L., Gadotti, D. A., Ferreira, L., et al. 2025, The evolution of the bar fraction and bar lengths in the last 12 billion years. https://arxiv.org/abs/2510.07407

    arXiv 2025

  27. [27]

    G., Guo, Y., et al

    Costantin, L., P´ erez-Gonz´ alez, P. G., Guo, Y., et al. 2023, Nature, 623, 499, doi: 10.1038/s41586-023-06636-x

    work page doi:10.1038/s41586-023-06636-x 2023

  28. [28]

    E., Whitaker, K

    Cutler, S. E., Whitaker, K. E., Weaver, J. R., et al. 2024, Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER. https://arxiv.org/abs/2312.15012

    arXiv 2024

  29. [29]

    P., Ness, M., Gonzalez, O

    Debattista, V. P., Ness, M., Gonzalez, O. A., et al. 2017, Monthly Notices of the Royal Astronomical Society, 469, 1587–1611, doi: 10.1093/mnras/stx947

    work page doi:10.1093/mnras/stx947 2017

  30. [30]

    P., & Sellwood, J

    Debattista, V. P., & Sellwood, J. A. 1998, The Astrophysical Journal, 493, L5–L8, doi: 10.1086/311118

    work page doi:10.1086/311118 1998

  31. [31]

    Cold streams in early massive hot haloes as the main mode of galaxy formation

    Dekel, A., Birnboim, Y., Engel, G., et al. 2009, Nature, 457, 451, doi: 10.1038/nature07648 D’Onghia, E. 2015, ApJL, 808, L8, doi: 10.1088/2041-8205/808/1/L8

    work page internal anchor Pith review doi:10.1038/nature07648 2009

  32. [32]

    S., Abraham, R

    Dunlop, J. S., Abraham, R. G., Ashby, M. L. N., et al. 2021, PRIMER: Public Release IMaging for Extragalactic

    2021

  33. [33]

    L., & Rankin, J

    Verdes-Montenegro, L. 2009, Monthly Notices of the Royal Astronomical Society, 397, 1756, doi: 10.1111/j.1365-2966.2009.15051.x

    work page doi:10.1111/j.1365-2966.2009.15051.x 2009

  34. [34]

    G., & Elmegreen, D

    Elmegreen, B. G., & Elmegreen, D. M. 1985, ApJ, 288, 438, doi: 10.1086/162810

    work page doi:10.1086/162810 1985

  35. [35]

    Erwin, P., & Sparke, L. S. 2002, The Astronomical Journal, 124, 65, doi: 10.1086/340803 Espejo Salcedo, J. M., Pastras, S., V´ acha, J., et al. 2025, A&A, 700, A42, doi: 10.1051/0004-6361/202554725

    work page doi:10.1086/340803 2002

  36. [36]

    2026, Formation timescales for stellar bars in diverse galactic discs

    Frosst, M., Obreschkow, D., & Ludlow, A. 2026, Formation timescales for stellar bars in diverse galactic discs. https://arxiv.org/abs/2602.21748

    arXiv 2026

  37. [37]

    S., et al., & et al

    Fruchter, A. S., et al., & et al. 2010, in 2010 Space Telescope Science Institute Calibration Workshop, 382–387

    2010

  38. [38]

    S., & Hook, R

    Fruchter, A. S., & Hook, R. N. 2002, PASP, 114, 144, doi: 10.1086/338393

    work page doi:10.1086/338393 2002

  39. [39]

    S., B´ edorf, J., Baba, J., & Portegies Zwart, S

    Fujii, M. S., B´ edorf, J., Baba, J., & Portegies Zwart, S. 2018, Monthly Notices of the Royal Astronomical Society, 477, 1451–1471, doi: 10.1093/mnras/sty711

    work page doi:10.1093/mnras/sty711 2018

  40. [40]

    Gadotti, D. A. 2011, Monthly Notices of the Royal Astronomical Society, 415, 3308, doi: 10.1111/j.1365-2966.2011.18945.x Gaia Collaboration, Vallenari, A., Brown, A. G. A., et al. 2023, A&A, 674, A1, doi: 10.1051/0004-6361/202243940

    work page doi:10.1111/j.1365-2966.2011.18945.x 2011

  41. [41]

    1991, A&AS, 89, 159 Garcia-G´ omez, C., Athanassoula, E., Barber` a, C., &

    Garcia-Gomez, C., & Athanassoula, E. 1991, A&AS, 89, 159 Garcia-G´ omez, C., Athanassoula, E., Barber` a, C., &

    1991

  42. [42]

    2017, A&A, 601, A132, doi: 10.1051/0004-6361/201628830

    Bosma, A. 2017, A&A, 601, A132, doi: 10.1051/0004-6361/201628830

    work page doi:10.1051/0004-6361/201628830 2017

  43. [43]

    2008, ApJ, 687, 59, doi: 10.1086/591840 Ivanov et al.23

    Genzel, R., Burkert, A., Bouch´ e, N., et al. 2008, ApJ, 687, 59, doi: 10.1086/591840 Ivanov et al.23

    work page doi:10.1086/591840 2008

  44. [44]

    Genzel, R., Schreiber, N. M. F., ¨Ubler, H., et al. 2017, Nature, 543, 397–401, doi: 10.1038/nature21685

    work page doi:10.1038/nature21685 2017

  45. [45]

    H., ¨Ubler, H., et al

    Genzel, R., Price, S. H., ¨Ubler, H., et al. 2020, The Astrophysical Journal, 902, 98, doi: 10.3847/1538-4357/abb0ea

    work page doi:10.3847/1538-4357/abb0ea 2020

  46. [46]

    2023, A&A, 674, A128, doi: 10.1051/0004-6361/202245275

    Ghosh, S., Fragkoudi, F., Di Matteo, P., & Saha, K. 2023, A&A, 674, A128, doi: 10.1051/0004-6361/202245275

    work page doi:10.1051/0004-6361/202245275 2023

  47. [47]

    Gould, K. M. L., Brammer, G., Valentino, F., et al. 2023, AJ, 165, 248, doi: 10.3847/1538-3881/accadc

    work page doi:10.3847/1538-3881/accadc 2023

  48. [48]

    A., Kocevski, D

    Grogin, N. A., Kocevski, D. D., Faber, S. M., et al. 2011, The Astrophysical Journal Supplement Series, 197, 35, doi: 10.1088/0067-0049/197/2/35

    work page doi:10.1088/0067-0049/197/2/35 2011

  49. [49]

    L., et al

    Guo, Y., Jogee, S., Finkelstein, S. L., et al. 2023, The Astrophysical Journal Letters, 945, L10, doi: 10.3847/2041-8213/acacfb

    work page doi:10.3847/2041-8213/acacfb 2023

  50. [50]

    2025, ApJ, 985, 181, doi: 10.3847/1538-4357/adc8a7 G´ eron, T., Smethurst, R

    Guo, Y., Jogee, S., Wise, E., et al. 2025, ApJ, 985, 181, doi: 10.3847/1538-4357/adc8a7 G´ eron, T., Smethurst, R. J., Dickinson, H., et al. 2025, The Astrophysical Journal, 987, 74, doi: 10.3847/1538-4357/add7d0

    work page doi:10.3847/1538-4357/adc8a7 2025

  51. [51]

    2025, Nature, 641, 861, doi: 10.1038/s41586-025-08914-2

    Huang, S., Kawabe, R., Umehata, H., et al. 2025, Nature, 641, 861, doi: 10.1038/s41586-025-08914-2

    work page doi:10.1038/s41586-025-08914-2 2025

  52. [52]

    2023, The Astrophysical Journal Letters, 958, L26, doi: 10.3847/2041-8213/acff63

    Huang, S., Kawabe, R., Kohno, K., et al. 2023, The Astrophysical Journal Letters, 958, L26, doi: 10.3847/2041-8213/acff63

    work page doi:10.3847/2041-8213/acff63 2023

  53. [53]

    2025, arXiv e-prints, arXiv:2502.03532, doi: 10.48550/arXiv.2502.03532

    Huertas-Company, M., Shuntov, M., Dong, Y., et al. 2025, arXiv e-prints, arXiv:2502.03532, doi: 10.48550/arXiv.2502.03532

    work page doi:10.48550/arxiv.2502.03532 2025

  54. [54]

    2024, A grand-design spiral galaxy 1.5 billion years after the Big Bang with JWST

    Jain, R., & Wadadekar, Y. 2024, A grand-design spiral galaxy 1.5 billion years after the Big Bang with JWST. https://arxiv.org/abs/2412.04834

    arXiv 2024

  55. [55]

    2006, in Physics of Active Galactic Nuclei at all Scales, ed

    Jogee, S. 2006, in Physics of Active Galactic Nuclei at all Scales, ed. D. Alloin, Vol. 693, 143, doi: 10.1007/3-540-34621-X 6

    work page doi:10.1007/3-540-34621-x 2006

  56. [56]

    Jogee, S., Scoville, N., & Kenney, J. D. P. 2005, The Astrophysical Journal, 630, 837, doi: 10.1086/432106

    work page doi:10.1086/432106 2005

  57. [57]

    D., Rix, H.-W., et al

    Jogee, S., Barazza, F. D., Rix, H.-W., et al. 2004, The Astrophysical Journal, 615, L105, doi: 10.1086/426138

    work page doi:10.1086/426138 2004

  58. [58]

    A., & Mandel, E

    Joye, W. A., & Mandel, E. 2003, in Astronomical Society of the Pacific Conference Series, Vol. 295, Astronomical Data Analysis Software and Systems XII, ed. H. E

    2003

  59. [59]

    M., Faber, S

    Koekemoer, A. M., Faber, S. M., Ferguson, H. C., et al. 2011, ApJS, 197, 36, doi: 10.1088/0067-0049/197/2/36

    work page doi:10.1088/0067-0049/197/2/36 2011

  60. [60]

    2013, Secular Evolution in Disk Galaxies

    Kormendy, J. 2013, Secular Evolution in Disk Galaxies. https://arxiv.org/abs/1311.2609

    Pith/arXiv arXiv 2013

  61. [61]

    Kormendy, J., & Kennicutt, Jr., R. C. 2004, ARA&A, 42, 603, doi: 10.1146/annurev.astro.42.053102.134024

    work page doi:10.1146/annurev.astro.42.053102.134024 2004

  62. [62]

    E., Reddy, N

    Kriek, M., Shapley, A. E., Reddy, N. A., et al. 2015, ApJS, 218, 15, doi: 10.1088/0067-0049/218/2/15

    work page doi:10.1088/0067-0049/218/2/15 2015

  63. [63]

    2024, The Astrophysical Journal Letters, 968, L15, doi: 10.3847/2041-8213/ad43eb

    Kuhn, V., Guo, Y., Martin, A., et al. 2024, The Astrophysical Journal Letters, 968, L15, doi: 10.3847/2041-8213/ad43eb

    work page doi:10.3847/2041-8213/ad43eb 2024

  64. [64]

    , year = 2005, month = apr, volume =

    Laurikainen, E., Salo, H., & Buta, R. 2005, Monthly Notices of the Royal Astronomical Society, 362, 1319, doi: 10.1111/j.1365-2966.2005.09404.x Le Conte, Z. A., Gadotti, D. A., Ferreira, L., et al. 2024, Monthly Notices of the Royal Astronomical Society, 530, 1984, doi: 10.1093/mnras/stae921

    work page doi:10.1111/j.1365-2966.2005.09404.x 2005

  65. [65]

    Lucey, M., Pearson, S., Hunt, J. A. S., et al. 2023, Monthly Notices of the Royal Astronomical Society, 520, 4779, doi: 10.1093/mnras/stad406

    work page doi:10.1093/mnras/stad406 2023

  66. [66]

    2007, ApJ, 659, 1176, doi: 10.1086/512355

    Marinova, I., & Jogee, S. 2007, ApJ, 659, 1176, doi: 10.1086/512355

    work page doi:10.1086/512355 2007

  67. [67]

    Daniel, K. J. 2025, Monthly Notices of the Royal Astronomical Society, 537, 1475, doi: 10.1093/mnras/staf107

    work page doi:10.1093/mnras/staf107 2025

  68. [68]

    M., Long, A

    McKinney, J., Casey, C. M., Long, A. S., et al. 2024, SCUBADive I: JWST+ALMA Analysis of 289 sub-millimeter galaxies in COSMOS-Web. https://arxiv.org/abs/2408.08346

    arXiv 2024

  69. [69]

    S., Steidel, C

    McLean, I. S., Steidel, C. C., Epps, H. W., et al. 2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 8446, Ground-based and Airborne Instrumentation for Astronomy IV, ed. I. S

    2012

  70. [70]

    McLean, S. K. Ramsay, & H. Takami, 84460J, doi: 10.1117/12.924794 Men´ endez-Delmestre, K., Sheth, K., Schinnerer, E., Jarrett, T. H., & Scoville, N. Z. 2007, ApJ, 657, 790, doi: 10.1086/511025 Men´ endez-Delmestre, K., Gon¸ calves, T. S., Sheth, K., et al. 2024, Monthly Notices of the Royal Astronomical Society, 527, 11777, doi: 10.1093/mnras/stad3662

    work page doi:10.1117/12.924794 2007

  71. [71]

    G., Brammer, G

    Momcheva, I. G., Brammer, G. B., van Dokkum, P. G., et al. 2016, ApJS, 225, 27, doi: 10.3847/0067-0049/225/2/27

    work page doi:10.3847/0067-0049/225/2/27 2016

  72. [72]

    2023, in American Astronomical Society Meeting Abstracts, Vol

    Mukundan, K., Nair, P., Masters, K., & Bailin, J. 2023, in American Astronomical Society Meeting Abstracts, Vol. 241, American Astronomical Society Meeting Abstracts, 177.67

    2023

  73. [73]

    1987, Monthly Notices of the Royal Astronomical Society, 228, 635, doi: 10.1093/mnras/228.3.635

    Noguchi, M. 1987, Monthly Notices of the Royal Astronomical Society, 228, 635, doi: 10.1093/mnras/228.3.635

    work page doi:10.1093/mnras/228.3.635 1987

  74. [74]

    1990, ApJ, 357, 71, doi: 10.1086/168892

    Ohta, K., Hamabe, M., & Wakamatsu, K.-I. 1990, ApJ, 357, 71, doi: 10.1086/168892

    work page doi:10.1086/168892 1990

  75. [75]

    P., & Peebles, P

    Ostriker, J. P., & Peebles, P. J. E. 1973, ApJ, 186, 467, doi: 10.1086/152513 24Ivanov et al

    work page doi:10.1086/152513 1973

  76. [76]

    Y., Ho, L

    Peng, C. Y., Ho, L. C., Impey, C. D., & Rix, H.-W. 2002, The Astronomical Journal, 124, 266–293, doi: 10.1086/340952 —. 2010, The Astronomical Journal, 139, 2097–2129, doi: 10.1088/0004-6256/139/6/2097

    work page internal anchor Pith review doi:10.1086/340952 2002

  77. [77]

    H., Shimizu, T

    Price, S. H., Shimizu, T. T., Genzel, R., et al. 2021, The Astrophysical Journal, 922, 143, doi: 10.3847/1538-4357/ac22ad Rodr´ ıguez, S., & Padilla, N. D. 2013, MNRAS, 434, 2153, doi: 10.1093/mnras/stt1168

    work page doi:10.3847/1538-4357/ac22ad 2021

  78. [78]

    , keywords =

    Rosas-Guevara, Y., Bonoli, S., Dotti, M., et al. 2022, MNRAS, 512, 5339, doi: 10.1093/mnras/stac816

    work page doi:10.1093/mnras/stac816 2022

  79. [79]

    Ryden, B. S. 2004, ApJ, 601, 214, doi: 10.1086/380437

    work page doi:10.1086/380437 2004

  80. [80]

    2013, Monthly Notices of the Royal Astronomical Society, 434, 1287, doi: 10.1093/mnras/stt1088

    Saha, K., & Naab, T. 2013, Monthly Notices of the Royal Astronomical Society, 434, 1287, doi: 10.1093/mnras/stt1088

    work page doi:10.1093/mnras/stt1088 2013

Showing first 80 references.