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arxiv: 2604.20411 · v1 · submitted 2026-04-22 · 🌌 astro-ph.GA

Recognition: unknown

The Evolution of the SFR-M_* relation at 0.1<z<4: Environmental and Morphological Dependencies

Jun Toshikawa, Kaimin He, Ke Shi, Xianzhong Zheng, Xiaopeng You

Authors on Pith no claims yet

Pith reviewed 2026-05-10 00:02 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords star formation ratestellar mass relationgalaxy morphologyenvironmental densityquenchinggalaxy evolutionhigh redshiftmorphological quenching
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The pith

Galaxy morphology regulates star formation rates at fixed stellar mass across redshifts, while environment primarily increases the quiescent fraction at low z.

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

The paper examines how star formation rate depends on stellar mass from redshift 0.1 to 4 using a large sample from the COSMOS2020 catalog. It finds that the relation shows a high-mass decline that grows stronger toward lower redshifts. This decline arises because bulge components in galaxies suppress star formation efficiency continuously, even among galaxies still forming stars. In contrast, living in dense environments suppresses star formation mainly by turning more galaxies quiescent at z less than 1, without changing the relation for those that remain star-forming. A reader would care because this distinguishes internal structural drivers from external environmental ones in how galaxies stop forming stars.

Core claim

The SFR-M_* relation exhibits a pronounced high-mass decline that becomes increasingly evident at lower redshifts. Examining environmental and morphological dependencies reveals that galaxies in high-density environments show suppressed star formation rates at z < 1, particularly at the high-mass end, but this effect vanishes when restricting to star-forming galaxies. Galaxy morphology, however, strongly influences the relation at z < 2, with early-type galaxies having lower star formation rates at fixed mass than spirals and irregulars, and this holds even within the star-forming population. These patterns indicate that internal structural properties, especially bulges, continuously regu

What carries the argument

morphological quenching driven by bulge components, which suppress star formation rates at fixed stellar mass independently of whether a galaxy is classified as star-forming or quiescent

If this is right

  • Internal bulge properties regulate star formation efficiency continuously from z=4 to z=0.1.
  • Environmental density suppresses overall star formation at low redshifts by increasing the number of quiescent galaxies rather than lowering rates in active ones.
  • The observed high-mass decline in the SFR-M_* relation results from better detection of massive galaxies experiencing morphological quenching.
  • Early-type galaxies show lower SFR at fixed mass even among star-forming systems at z<2.

Where Pith is reading between the lines

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

  • If bulge growth is the main regulator, then the SFR-M_* relation should flatten at high masses in samples where bulge fractions are controlled for.
  • This separation of mechanisms implies that simulations of galaxy evolution must treat morphological transformation and environmental effects as distinct quenching channels.
  • Extending this to higher redshifts or other fields could test whether morphological regulation strengthens as the universe ages.
  • Neighbouring problems like the morphology-density relation may partly arise from environment increasing quiescent fractions rather than directly altering morphologies.

Load-bearing premise

The COSMOS2020 catalog provides an unbiased, mass-complete sample at high stellar masses with accurate morphology and environment classifications free of selection effects that might create an artificial high-mass decline.

What would settle it

A survey finding that star-forming early-type galaxies have the same SFR-M_* relation as late-type ones at high masses and z<2, or that dense environments suppress SFR equally in star-forming galaxies, would challenge the distinction between internal and external effects.

Figures

Figures reproduced from arXiv: 2604.20411 by Jun Toshikawa, Kaimin He, Ke Shi, Xianzhong Zheng, Xiaopeng You.

Figure 1
Figure 1. Figure 1: SFR-M⋆ relations for all galaxies (left panel) and star-forming galaxies (right panel). The median SFR in each mass bin are plotted with errorbars denoting the median absolute deviations. Solid lines represent the best-fit relations of Equation 1. Bottom panels show the residuals calculated as the difference between the measured and best-fit log(SFR) values. 3.2. Redshift evolution of model parameters [PI… view at source ↗
Figure 2
Figure 2. Figure 2: Redshift evolution of the best-fit parameters for all galax [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Left: the cosmic SFRD as a function of stellar mass at di [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Redshift evolution of the cosmic star-formation rate den [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Environmental dependence of the SFR￾M⋆ relation for all galaxies. The upper seven panels show the SFR-M⋆ relation in each red￾shift bin for all galaxies in different local den￾sities as defined in the text. The best-fit rela￾tion for all galaxies in [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Same as [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Quiescent fraction as a function of redshift in di [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: SFR-M⋆ relation for all galaxies with different morphology types. The upper seven panels show the SFR-M⋆ relation in each red￾shift bin for all galaxies of different morpholo￾gies as defined in the text. The best-fit relation for all galaxies in [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Same as [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Quiescent fraction as a function of redshift for di [PITH_FULL_IMAGE:figures/full_fig_p010_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Star-forming main sequence relation compared with literature at di [PITH_FULL_IMAGE:figures/full_fig_p012_11.png] view at source ↗
read the original abstract

We present a comprehensive study of the relationship between star formation rate (SFR) and stellar mass (M_*) from z = 0.1 to z = 4 using a mass-complete sample of approximately 290,000 galaxies from the COSMOS2020 catalog. We find that the SFR-M_* relation exhibits a pronounced high-mass decline that becomes increasingly evident at lower redshifts. Examining environmental and morphological dependencies, we find strikingly different patterns. For all galaxies, we find galaxies in high-density environments exhibit suppressed star formation rates at z < 1 especially at high-mass end, while for star-forming galaxies no apparent environmental effect is found at all redshifts. In contrast, galaxy morphology exerts strong influence on the SFR-M_* relation at z < 2, in a sense that early-type galaxies exhibit systematically lower star formation rates at fixed mass compared to spirals and irregulars, with this trend persisting even within the star-forming population. These results suggest that internal structural properties (bulge components in particular) continuously regulate star formation efficiency independently of whether galaxies are classified as active or quiescent, whereas external environmental processes primarily serve as rapid quenching mechanisms that increase the fraction of quiescent galaxies at low redshifts. We attribute the observed high-mass decline of the SFR-M_* relation to COSMOS2020's superior capability for detecting massive star-forming galaxies undergoing "morphological quenching" processes.

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 the SFR-M_* relation over 0.1 < z < 4 using a mass-complete sample of ~290,000 galaxies from the COSMOS2020 catalog. It reports a high-mass decline that strengthens toward lower redshifts, environmental suppression of SFR at z < 1 (high-density regions, high-mass end) for the full population but no effect within star-forming galaxies, and a strong morphological dependence (early-types lower SFR than spirals/irregulars) that persists even inside the star-forming subsample. The authors conclude that bulge-driven internal regulation acts continuously on star-formation efficiency while environment primarily boosts the quiescent fraction, and they attribute the high-mass decline to COSMOS2020's improved detection of massive morphologically-quenched star-forming galaxies.

Significance. If the sample completeness, morphological classifications, and SFR measurements prove robust, the work supplies a large-statistic observational separation between internal structural and external environmental quenching channels across a wide redshift range. The finding that morphology affects the SFR-M_* slope even among star-forming galaxies, while environment does not, would provide a useful benchmark for simulations and semi-analytic models that currently struggle to reproduce the high-mass end of the star-forming main sequence.

major comments (3)
  1. [§2] §2 (Data and Sample Selection): The central claim that the high-mass decline reflects genuine morphological quenching rather than catalog selection requires explicit demonstration that the COSMOS2020 sample remains mass-complete and unbiased at M_* ≳ 10^11 M_⊙ for star-forming galaxies across morphological types. Without completeness simulations or recovery fractions as a function of morphology, SFR, and environment, the differential patterns (environment affects all galaxies but not SF-only; morphology affects both) could arise from mass-dependent detection or SED-fitting biases.
  2. [§4.3] §4.3 (Morphological Dependencies): The persistence of the morphological trend inside the star-forming population is load-bearing for the conclusion of continuous internal regulation. The manuscript should quantify how sensitive this result is to the precise morphological classification method (e.g., visual vs. parametric vs. machine-learning) and to the SFR threshold used to define the star-forming subsample; small changes in either could alter the reported early-type vs. late-type offset at fixed mass.
  3. [§5] §5 (Interpretation and High-Mass Decline): The attribution of the high-mass decline specifically to COSMOS2020's superior detection of morphologically quenched galaxies needs a direct comparison with shallower or differently selected catalogs (e.g., UltraVISTA or 3D-HST) at overlapping redshifts and masses to rule out survey-specific systematics.
minor comments (2)
  1. [Figures] Figure 3 and 4: Axis labels and legend entries for environmental density bins should explicitly state the percentile or surface-density thresholds used; current notation is ambiguous for readers attempting to reproduce the bins.
  2. Throughout: The term 'early-type' is used interchangeably with 'bulge-dominated'; a brief clarification of the exact morphological criteria (e.g., Sérsic index cut or visual class) would improve clarity.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed comments, which have prompted us to strengthen several aspects of the analysis and presentation. We respond to each major comment below and have made revisions to the manuscript to address the concerns raised.

read point-by-point responses

  1. Referee: [§2] §2 (Data and Sample Selection): The central claim that the high-mass decline reflects genuine morphological quenching rather than catalog selection requires explicit demonstration that the COSMOS2020 sample remains mass-complete and unbiased at M_* ≳ 10^11 M_⊙ for star-forming galaxies across morphological types. Without completeness simulations or recovery fractions as a function of morphology, SFR, and environment, the differential patterns (environment affects all galaxies but not SF-only; morphology affects both) could arise from mass-dependent detection or SED-fitting biases.

    Authors: We agree that explicit verification of completeness across morphology and SFR is important for supporting the interpretation. The COSMOS2020 catalog (Weaver et al. 2022) already provides mass-completeness limits and recovery fractions based on extensive simulations, with >90% completeness for M_* > 10^{10.5} M_⊙ at z < 4. To further address morphology- and SFR-dependent biases, we have added a dedicated paragraph in §2 together with a supplementary figure showing recovery fractions derived from the catalog's mock catalogs, stratified by morphological type and SFR. These tests indicate that the high-mass decline persists even after accounting for selection effects, and we have clarified that the differential environmental and morphological trends are unlikely to be driven by catalog biases. revision: yes

  2. Referee: [§4.3] §4.3 (Morphological Dependencies): The persistence of the morphological trend inside the star-forming population is load-bearing for the conclusion of continuous internal regulation. The manuscript should quantify how sensitive this result is to the precise morphological classification method (e.g., visual vs. parametric vs. machine-learning) and to the SFR threshold used to define the star-forming subsample; small changes in either could alter the reported early-type vs. late-type offset at fixed mass.

    Authors: We concur that demonstrating robustness to classification choices and SFR definition is essential. We have performed additional sensitivity tests: (i) cross-comparing our machine-learning morphologies with available visual and parametric classifications for overlapping subsamples, and (ii) shifting the star-forming threshold by ±0.3 dex around the adopted cut. In all variants the early-type offset at fixed mass remains significant (>3σ) within the star-forming population. These results have been quantified in a new subsection of §4.3, including a supplementary table summarizing the offsets under different choices. revision: yes

  3. Referee: [§5] §5 (Interpretation and High-Mass Decline): The attribution of the high-mass decline specifically to COSMOS2020's superior detection of morphologically quenched galaxies needs a direct comparison with shallower or differently selected catalogs (e.g., UltraVISTA or 3D-HST) at overlapping redshifts and masses to rule out survey-specific systematics.

    Authors: We have added a direct comparison in the revised §5 with the SFR-M_* relations from 3D-HST (at 1 < z < 2) and UltraVISTA (at z < 1) over the same mass range. The comparison, now shown in a new figure, confirms that the high-mass decline is more pronounced in COSMOS2020 while the overall normalization agrees within uncertainties, consistent with COSMOS2020's deeper imaging and improved morphological classification enabling detection of massive star-forming galaxies with bulge components. We have updated the discussion to incorporate this cross-survey check. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational catalog analysis

full rationale

The paper is an empirical study that measures the SFR-M_* relation and its dependencies directly from the COSMOS2020 catalog sample of ~290k galaxies. No equations, fitted parameters, or derivations are present that could reduce outputs to inputs by construction. Environmental and morphological trends are reported as observed patterns in the data, with interpretations following from those patterns rather than from any self-referential definitions, predictions of fitted quantities, or load-bearing self-citations. The analysis is self-contained against external catalog benchmarks and does not invoke uniqueness theorems or ansatzes from prior author work.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claims rest on the assumption that the COSMOS2020 catalog delivers a mass-complete sample with reliable morphological and environmental classifications; no free parameters or invented entities are introduced in the abstract.

axioms (1)
  • domain assumption COSMOS2020 catalog provides a mass-complete sample of approximately 290,000 galaxies suitable for SFR-M_* analysis across 0.1<z<4
    Stated directly in the abstract as the basis for the study

pith-pipeline@v0.9.0 · 5567 in / 1158 out tokens · 41715 ms · 2026-05-10T00:02:01.179160+00:00 · methodology

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Reference graph

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