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arxiv: 2606.21651 · v1 · pith:VIGI5MWTnew · submitted 2026-06-19 · 🌌 astro-ph.GA

Resolved Ages and Stellar Metallicities in Progenitors of Milky Way Analogs: A Closer Look at their Star Formation Histories since z=5

Vivian Yun Yan Tan , Adam Muzzin , Naadiyah Jagga , Visal Sok , Ghassan T. E. Sarrouh , Gregor Rihtar\v{s}i\v{c} , Roberto Abraham , Yoshihisa Asada
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Maru\v{s}a Brada\v{c} Kartheik Iyer Nicholas S. Martis Ga\"el Noirot Marcin Sawicki Chris J. Willott Sunna Withers
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Pith reviewed 2026-06-26 13:31 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Milky Way analogsinside-out assemblygalaxy mergersstellar metallicitystar formation historiesresolved SED fittinggalaxy evolutionCANUCS survey
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The pith

Milky Way analog galaxies assemble mass inside-out from z=5, with major mergers causing only temporary gradient disruptions.

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

The paper tracks resolved mass-weighted ages, stellar metallicities, and specific star formation rates in 872 Milky Way analog progenitors from redshift 5 using CANUCS data. Non-merging galaxies show negative or flat age gradients and positive or flat sSFR gradients at all epochs, matching the signature of inside-out disk growth. Mergers display flatter age gradients and more negative sSFR gradients, yet the overall inside-out pattern remains intact across cosmic time.

Core claim

Non-mergers exhibit average age gradients from -0.022 to 0.005 dex/kpc and sSFR gradients from -0.089 to 0.092 dex/kpc, consistent with inside-out assembly, while metallicity gradients range from -0.029 to 0.044 dex/kpc with positive values appearing only at 2<z<3. Mergers show flatter age gradients, more negative sSFR gradients, and comparable metallicity gradients at every redshift. Splitting merger components reveals similar ages and metallicities between galaxies but 0.1-0.4 dex higher sSFR in the less massive component.

What carries the argument

Spatially resolved SED fitting with the non-parametric Dense Basis code applied to CANUCS imaging, combined with Gini-M20 analysis on stellar mass maps via Statmorph to classify ongoing major mergers.

If this is right

  • Non-merger MWA progenitors follow inside-out mass assembly at every redshift from z=5 to the present.
  • Major mergers produce flatter age gradients and steeper negative sSFR gradients but do not reverse the long-term inside-out trend.
  • Merging galaxy pairs maintain similar average ages and metallicities between components.
  • The less massive merger component maintains elevated sSFR relative to its partner at all epochs examined.

Where Pith is reading between the lines

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

  • Galaxy formation models must accommodate short-lived merger-driven star-formation enhancements that leave the radial growth direction unchanged.
  • Higher-resolution imaging at 2<z<3 could test whether the observed positive metallicity gradients trace specific gas-accretion events.
  • The Milky Way's own disk likely experienced similar inside-out growth punctuated by occasional major-merger interruptions.

Load-bearing premise

The Gini-M20 parameter measured on stellar mass maps correctly separates major mergers from non-mergers, and the CANUCS sample galaxies are representative Milky Way analogs whose SED-derived ages and metallicities carry no strong systematic bias from dust or assumed star-formation histories.

What would settle it

A sample of non-merger Milky Way analogs showing positive age gradients across multiple redshift bins or lacking inside-out signatures in aggregate would falsify the central claim.

Figures

Figures reproduced from arXiv: 2606.21651 by Adam Muzzin, Chris J. Willott, Ga\"el Noirot, Ghassan T. E. Sarrouh, Gregor Rihtar\v{s}i\v{c}, Kartheik Iyer, Marcin Sawicki, Maru\v{s}a Brada\v{c}, Naadiyah Jagga, Nicholas S. Martis, Roberto Abraham, Sunna Withers, Visal Sok, Vivian Yun Yan Tan, Yoshihisa Asada.

Figure 1
Figure 1. Figure 1: Top panel: Integrated stellar mass of all star-forming MWA progenitors in our sample from the CANUCS DR1 catalogs (G. T. E. Sarrouh et al. 2025), as a function of redshift. their color indicates specific star formation rate (sSFR). Bottom left: Gini-M20 distribution of our sample. Yellow squares are non-mergers, red diamonds are late stage mergers, blue circles are ongoing mergers. The three non-yellow poi… view at source ↗
Figure 2
Figure 2. Figure 2: Color image, SFHs and property maps (left to right, stellar mass density, SFR density, dust attenuation, stellar metallicity, mass-weighted age) for two example galaxies at redshift ranges 1 < z < 2, top is a merger, bottom is a non-merger. Every spatial bin’s SFH (SFR/yr/pixel) is plotted grey. The blue line is the median SFH, while shaded region is the 1σ deviation of the same SFHs. The empty region at t… view at source ↗
Figure 3
Figure 3. Figure 3: Color image and property maps for two galaxies at redshift ranges 4 < z < 5, top is a non-merger, bottom is a merger. formed mass will be returned to the interstellar medium via stellar evolution. Then we obtain the mass-weighted age tMW age by multiplying the age ti at each time step by its corresponding Mformed at ti , taking the sum, and then dividing by the total mass formed over all time: tMW age = Pt… view at source ↗
Figure 4
Figure 4. Figure 4: Median mass-weighted age (top panel, stellar metallicity (middle panel), and sSFR (bottom panel) of the inner 1Reff (half-light radius) of the resolved MWA progen￾itor sample for every redshift bin. Error bars are the 1σ scat￾ters of the properties’ distributions. Open markers indicate bins affected by mass-incompleteness. The black solid lines and the grey shaded regions represent the median and the 1σ sc… view at source ↗
Figure 5
Figure 5. Figure 5: The average mass-weighted age gradients for each redshift epoch created by stacking and normalizing each mass-weighted age profile. The distance from the galactic center is shown in kpc. The shaded regions represent the 1σ scatter, or the 16th-84th percentile range of the properties. Left panel is the non-merger sample, middle are ongoing mergers, and right panel are late stage mergers. Dashed lines indica… view at source ↗
Figure 6
Figure 6. Figure 6: Similar plots as [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Similar plots as Figures 5 and 6, but for sSFR. Each radial gradient is on its own axis for visual clarity [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Slopes of the mass-weighted age (top panel), metallicity (middle panel) and sSFR density (bottom panel) gradients for each redshift bin. Yellow squares are non-merg￾ers, red diamonds are late stage mergers, blue circles are ongoing mergers. Error bars represent the fitting error in the slope, weighed by the scatter in the distribution. Open markers indicate bins affected by mass incompleteness. off” at a d… view at source ↗
Figure 9
Figure 9. Figure 9: Two examples of ongoing mergers being divided into separate regions, using the watershed algorithm on a combination of the Σ⋆ and ΣSF R maps. The first cutout is divided into two regions, and the second cutout is divided into three regions. From top left to top right: we display the color image with the regions overlaid on top, the Voronoi bins of all the regions, followed by the Voronoi bins of each separ… view at source ↗
Figure 10
Figure 10. Figure 10: Left Panel: Mass fractions of merger components. Error bar is the 1 − σ scatter. Right panels: Difference in average age, average metallicity and average sSFR of the components of the merger versus the average properties of the entire merger system. Errors are standard error of the mean for more visual clarity of the property differences as a function of redshift. The individual property differences for t… view at source ↗
Figure 11
Figure 11. Figure 11: Difference between the median log(ageMW ), log(Z/Z⊙), and sSFR of the late stage mergers, ongoing mergers, and the average values of the ongoing merger com￾ponents. Median values for the radial profile measurements come from [PITH_FULL_IMAGE:figures/full_fig_p015_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Top Left Panel: Light-weighted [Fe/H] radial gradients of the MW from J. Lian et al. (2023). Dashed lines are the slope fitted to the gradients of the respective colors. Top Right Panel: Median [Mg/Fe] vs [Fe/H] distributions for MW disk stars for high-α and low-α populations, colours represent radial distance in steps of 2 kpc, adapted from [PITH_FULL_IMAGE:figures/full_fig_p016_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Stacked and normalized property gradients at each redshift bin, similar to Figures 5, 6 and 7, but as a function of the galaxy’s effective radius (Reff ) instead of kpc [PITH_FULL_IMAGE:figures/full_fig_p023_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Slopes of property gradients as a function of redshift in units of dex/Reff . Overall, the slopes have similar evolution with redshift, but the magnitude of the slope is larger when measured in Reff than in kpc. Additionally, if this degeneracy has a noticeable effect on the properties of galaxies, we would expect the ra￾dial profile of dust to be the inverse of either the age or the metallicity gradient.… view at source ↗
Figure 15
Figure 15. Figure 15: Top row: Corner plots of dust, metallicity, and stellar age for spatial bins of galaxies in the CLU fields versus the NCF fields. Bottom rows are similar corner plots but between smaller sized central bins (bin size ≤ 5 pixels), versus larger, less central bins (bin size > 5 pixels). The 2D contours are for 1σ, 1.5σ, and 2σ confidence intervals [PITH_FULL_IMAGE:figures/full_fig_p025_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Top panel: The radial dust attentuation (AV transmission) gradient of each galaxy in our sample, separated into eight redshift bins, as a function of kpc. Solid colored lines in each subplot represent the stacked and normalized average of that redshift bin. Shaded regions is the 1σ scatter, or the 18th-84th percentile. Thin grey lines are the individual dust gradients for non-mergers, thin blue lines are … view at source ↗
read the original abstract

We present the evolution of the resolved mass-weighted age, stellar metallicity, and sSFR of 872 Milky Way Analog (MWA) progenitors up to redshift $z=5$ from the Canadian Unbiased Cluster Survey (CANUCS). The metallicity and mass-weighted ages were obtained via spatially resolved SED-fitting with the non-parametric code Dense Basis. We split the sample into mergers versus non-mergers using the merger parameter from the Gini-$M_{20}$ plane obtained through Gini-$M_{20}$ analysis of the morphology of the stellar mass maps with Statmorph. Across our redshift range, non-mergers have negative or flat average age gradients from $-0.022$ to 0.005 dex/kpc, and positive or flat sSFR gradients from $-0.089$ to 0.092 dex/kpc, consistent with inside-out assembly. The average $\log(Z/\Zsun)$ gradients for non-mergers range from $-0.029$ to 0.044 dex/kpc, however, positive gradients only appear between $2 < z < 3$. At every redshift epoch, mergers typically have flatter age gradients, more negative sSFR gradients, and similar metallicity gradients compared to non-mergers. We divide the property maps of ongoing mergers into separate regions based on their component galaxies, and find little to no difference between the components' average ages or metallicities, but the less massive of the merging system is on average $0.1-0.4$ dex higher in sSFR. Our results point to major mergers contributing some momentary disruption to the general trend of inside-out mass assembly, but does not upend the overall picture of MWA disks growing inside-out over cosmic time.

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

3 major / 2 minor

Summary. The manuscript analyzes resolved mass-weighted ages, stellar metallicities, and sSFR for 872 Milky Way analog (MWA) progenitors from the CANUCS survey up to z=5. Spatially resolved SED fitting is performed with the non-parametric Dense Basis code, and galaxies are classified as mergers or non-mergers via the Gini-M20 parameter measured on stellar mass maps using Statmorph. Non-mergers exhibit negative or flat age gradients (-0.022 to 0.005 dex/kpc) and positive or flat sSFR gradients, consistent with inside-out assembly; metallicity gradients range from -0.029 to 0.044 dex/kpc with positive values only at 2<z<3. Mergers show flatter age gradients, more negative sSFR gradients, and comparable metallicity gradients. Component analysis of mergers finds similar ages and metallicities but higher sSFR in the less massive component. The central conclusion is that major mergers produce momentary disruption to inside-out growth without overturning the overall picture for MWA disks.

Significance. If the results are robust, the work supplies a valuable high-redshift empirical benchmark on the role of major mergers in Milky Way-like disk assembly, using a large sample and direct comparison of resolved properties. The extension to z=5 and the use of non-parametric SED fitting to mitigate SFH assumptions are notable strengths that could inform semi-analytic models and simulations of inside-out growth.

major comments (3)
  1. [Abstract] Abstract and methods description of sample and classification: The claim that Gini-M20 on stellar mass maps reliably separates ongoing major mergers from non-mergers is load-bearing for all reported gradient differences, yet no validation against simulations, visual classification, or alternative merger indicators (e.g., close-pair statistics) is referenced; without this, the reported flatter age gradients and more negative sSFR gradients in mergers cannot be confidently attributed to merger status rather than classification systematics.
  2. [Abstract] Abstract and SED-fitting description: The reported age, metallicity, and sSFR gradients rest on Dense Basis fits whose sensitivity to dust attenuation, metallicity priors, and SFH assumptions at z>2 is not quantified via robustness tests or alternative codes; this directly affects the central inside-out assembly claim and the conclusion that mergers cause only 'momentary disruption'.
  3. [Abstract] Abstract: Average gradients are stated without per-bin uncertainties, bootstrap errors, or Kolmogorov-Smirnov test p-values comparing merger versus non-merger distributions; the absence of these statistics undermines the assertion that differences are systematic rather than consistent with noise, which is required to support the 'does not upend' conclusion.
minor comments (2)
  1. [Abstract] The abstract states '872 Milky Way Analog progenitors' but does not specify the exact redshift bin occupancies or the stellar-mass and morphological selection criteria used to define the MWA sample; adding a table or sentence with these numbers would improve reproducibility.
  2. Notation for gradients (dex/kpc) is clear, but the manuscript should explicitly state whether the reported averages are weighted by galaxy stellar mass or number of galaxies.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed comments, which help clarify the presentation and robustness of our results on resolved stellar properties in Milky Way analog progenitors. We address each major comment below and will revise the manuscript to incorporate additional validation, robustness checks, and statistical measures as outlined.

read point-by-point responses

  1. Referee: [Abstract] Abstract and methods description of sample and classification: The claim that Gini-M20 on stellar mass maps reliably separates ongoing major mergers from non-mergers is load-bearing for all reported gradient differences, yet no validation against simulations, visual classification, or alternative merger indicators (e.g., close-pair statistics) is referenced; without this, the reported flatter age gradients and more negative sSFR gradients in mergers cannot be confidently attributed to merger status rather than classification systematics.

    Authors: We agree that explicit validation strengthens the merger classification. While the Gini-M20 method on stellar mass maps follows established practices in the high-redshift literature, the current manuscript does not cite specific validation studies. In revision we will add references to simulation-based validations of Gini-M20 (including on mass maps) and discuss consistency with visual classifications and close-pair statistics where the CANUCS data permit. This will directly support attribution of the observed gradient differences to merger status. revision: yes

  2. Referee: [Abstract] Abstract and SED-fitting description: The reported age, metallicity, and sSFR gradients rest on Dense Basis fits whose sensitivity to dust attenuation, metallicity priors, and SFH assumptions at z>2 is not quantified via robustness tests or alternative codes; this directly affects the central inside-out assembly claim and the conclusion that mergers cause only 'momentary disruption'.

    Authors: We acknowledge the value of quantifying these sensitivities. Although Dense Basis is non-parametric and was chosen to reduce SFH priors, the manuscript does not present explicit robustness tests at z>2. In the revised version we will add a dedicated subsection reporting results from varying dust attenuation laws, metallicity priors, and comparisons with an alternative SED code on a subset of the sample, thereby confirming that the inside-out trends and merger disruption conclusions remain stable. revision: yes

  3. Referee: [Abstract] Abstract: Average gradients are stated without per-bin uncertainties, bootstrap errors, or Kolmogorov-Smirnov test p-values comparing merger versus non-merger distributions; the absence of these statistics undermines the assertion that differences are systematic rather than consistent with noise, which is required to support the 'does not upend' conclusion.

    Authors: We accept this point. The abstract and main text currently report mean gradients without accompanying uncertainties or formal statistical comparisons. In revision we will include bootstrap-derived uncertainties on all reported averages, per-redshift-bin error bars, and Kolmogorov-Smirnov p-values for the merger versus non-merger distributions. These additions will quantitatively support the claim that the differences are systematic. revision: yes

Circularity Check

0 steps flagged

No significant circularity

full rationale

This is a purely observational study that reports empirical measurements of resolved ages, metallicities, and sSFR gradients from CANUCS survey data. The analysis applies standard external tools (Dense Basis for non-parametric SED fitting; Statmorph for Gini-M20 morphology) to derive property maps and gradients directly from the observations. No derivation chain, fitted-parameter prediction, self-citation load-bearing step, or ansatz reduction is present; the central claims are data-driven comparisons between mergers and non-mergers across redshift bins. The paper is self-contained against external benchmarks with no internal reduction of results to inputs by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on the validity of non-parametric SED fitting assumptions and the accuracy of Gini-M20 merger classification; no free parameters or invented entities are explicitly introduced in the abstract.

axioms (2)
  • domain assumption Non-parametric SED fitting with Dense Basis recovers unbiased mass-weighted ages and metallicities for high-redshift galaxies despite dust and star-formation history degeneracies.
    Invoked to obtain the reported age and metallicity maps from CANUCS photometry.
  • domain assumption Gini-M20 parameter measured on stellar mass maps accurately identifies major mergers versus non-mergers.
    Used to split the sample and compare gradients.

pith-pipeline@v0.9.1-grok · 5947 in / 1384 out tokens · 30051 ms · 2026-06-26T13:31:27.522051+00:00 · methodology

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Reference graph

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