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The evolution of the galaxy stellar mass function over the last twelve billion years from a combination of ground-based and HST surveys
Astrophysics of Galaxies · Submitted 7 Sep 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find no evidence for significant evolution in $M^{\star}$, with the intrinsic value consistent with $\log_{10}(M^{\star} / M_{\odot})=10.55\pm{0.1}$ over the full redshift range.
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We present a new determination of the galaxy stellar mass function (GSMF) over the redshift interval $0.25 \leq z \leq 3.75$, derived from a combination of ground-based and Hubble Space Telescope (HST) imaging surveys. Based on a near-IR selected galaxy sample selected over a raw survey area of 3 deg$^{2}$ and spanning $\geq 4$ dex in stellar mass, we fit the GSMF with both single and double Schechter functions, carefully accounting for Eddington bias to derive both observed and intrinsic parameter values. We find that a double Schechter function is a better fit to the GSMF at all redshifts, although the single and double Schechter function fits are statistically indistinguishable by $z=3.25$. We find no evidence for significant evolution in $M^{\star}$, with the intrinsic value consistent with $\log_{10}(M^{\star} / M_{\odot})=10.55\pm{0.1}$ over the full redshift range. Overall, our determination of the GSMF is in good agreement with recent simulation results, although differences persist at the highest stellar masses. Splitting our sample according to location on the UVJ plane, we find that the star-forming GSMF can be adequately described by a single Schechter function over the full redshift range, and has not evolved significantly since $z\simeq 2.5$. In contrast, both the normalization and functional form of the passive GSMF evolves dramatically with redshift, switching from a single to a double Schechter function at $z \leq 1.5$. As a result, we find that while passive galaxies dominate the integrated stellar-mass density at $z \leq 0.75$, they only contribute $\lesssim 10$ per cent by $z\simeq 3$. Finally, we provide a simple parameterization that provides an accurate estimate of the GSMF, both observed and intrinsic, at any redshift within the range $0 \leq z \leq 4$.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present a new determination of the galaxy stellar mass function (GSMF) over the redshift interval $0.25 \leq z \leq 3.75$, derived from a combination of ground-based and Hubble Space Telescope (HST) imaging surveys. | contribution 1.00 | 0.97 | 0.06 | asserted 1.00 |
| s1 | Based on a near-IR selected galaxy sample selected over a raw survey area of 3 deg$^{2}$ and spanning $\geq 4$ dex in stellar mass, we fit the GSMF with both single and double Schechter functions, carefully accounting for Eddington bias to derive both observed and intrinsic parameter values. | method 1.00 | 0.96 | 0.04 | asserted 0.96 |
| s2 | We find that a double Schechter function is a better fit to the GSMF at all redshifts, although the single and double Schechter function fits are statistically indistinguishable by $z=3.25$. | result 1.00 | 0.97 | 0.18 | asserted 1.00 |
| s3 | We find no evidence for significant evolution in $M^{\star}$, with the intrinsic value consistent with $\log_{10}(M^{\star} / M_{\odot})=10.55\pm{0.1}$ over the full redshift range. | result 1.00 | 0.97 | 0.29 | asserted 0.93 |
| s4 | Overall, our determination of the GSMF is in good agreement with recent simulation results, although differences persist at the highest stellar masses. | interpretation 0.51 | 0.76 | 0.07 | asserted 0.94 |
| s5 | Splitting our sample according to location on the UVJ plane, we find that the star-forming GSMF can be adequately described by a single Schechter function over the full redshift range, and has not evolved significantly since $z\simeq 2.5$. | result 1.00 | 0.97 | 0.12 | asserted 1.00 |
| s6 | In contrast, both the normalization and functional form of the passive GSMF evolves dramatically with redshift, switching from a single to a double Schechter function at $z \leq 1.5$. | result 1.00 | 0.95 | 0.18 | asserted 1.00 |
| s7 | As a result, we find that while passive galaxies dominate the integrated stellar-mass density at $z \leq 0.75$, they only contribute $\lesssim 10$ per cent by $z\simeq 3$. | result 0.90 | 0.97 | 0.17 | asserted 1.00 |
| s8 | Finally, we provide a simple parameterization that provides an accurate estimate of the GSMF, both observed and intrinsic, at any redshift within the range $0 \leq z \leq 4$. | contribution 0.87 | 0.95 | 0.11 | asserted 1.00 |
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The paper
Original abstract
We present a new determination of the galaxy stellar mass function (GSMF) over the redshift interval $0.25 \leq z \leq 3.75$, derived from a combination of ground-based and Hubble Space Telescope (HST) imaging surveys. Based on a near-IR selected galaxy sample selected over a raw survey area of 3 deg$^{2}$ and spanning $\geq 4$ dex in stellar mass, we fit the GSMF with both single and double Schechter functions, carefully accounting for Eddington bias to derive both observed and intrinsic parameter values. We find that a double Schechter function is a better fit to the GSMF at all redshifts, although the single and double Schechter function fits are statistically indistinguishable by $z=3.25$. We find no evidence for significant evolution in $M^{\star}$, with the intrinsic value consistent with $\log_{10}(M^{\star} / M_{\odot})=10.55\pm{0.1}$ over the full redshift range. Overall, our determination of the GSMF is in good agreement with recent simulation results, although differences persist at the highest stellar masses. Splitting our sample according to location on the UVJ plane, we find that the star-forming GSMF can be adequately described by a single Schechter function over the full redshift range, and has not evolved significantly since $z\simeq 2.5$. In contrast, both the normalization and functional form of the passive GSMF evolves dramatically with redshift, switching from a single to a double Schechter function at $z \leq 1.5$. As a result, we find that while passive galaxies dominate the integrated stellar-mass density at $z \leq 0.75$, they only contribute $\lesssim 10$ per cent by $z\simeq 3$. Finally, we provide a simple parameterization that provides an accurate estimate of the GSMF, both observed and intrinsic, at any redshift within the range $0 \leq z \leq 4$.
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References
How later papers used it
71 later papers cite it
4 later papers by other authors are listed below: 2 used its data or values and 2 compared their own results with it. 1 more paper by the same authors is listed: 1 used its method or tool.
Uses its method or tool 1 of 4 papers with this label · 1 by the same authors
By the same authors
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The catalogue construction follows the methods employed in [ref] .
Galaxy clusters in the VIDEO fields: detection and characterisation in the context of MOONRISE (2026) (same authors) · The VIDEO catalogues of galaxies · 1.00
Uses its data or values 2 of 8 papers with this label
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Then the fraction of each $L_$-selected subsample at a given stellar mass is defined as [equation] where the number density $n( )$ of all galaxies for a stellar mass bin can by estimated by integrating the galaxy stellar mass function (SMF) $Φ()$: [equation] Here we adopt the SMF measured by [ref] in the redshift range $0.25<z<0.75$.
Construct the emission line galaxy-host halo connection through auto and cross correlations (2021) · ELG-stellar mass relation in the observation · 0.99
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Used the single-Schechter intrinsic SMF at 0.75<z<1.25 from this paper.
The assembly of supermassive black holes at $z<1$ in early-type galaxies from scaling relations (2025) · 0.87 · paraphrased: the licence does not allow quoting
Compares with it 2 of 11 papers with this label
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At all masses shown in this redshift range, the SMF of our sample lies below the pre-JWST SMF from [ref] [ref] and [ref] (based on HST and ground-based observations).
Unveiling the hidden universe with JWST: The contribution of dust-obscured galaxies to the stellar mass function at $z\sim3-8$ (2023) · SMFs at $3<𝐳<8$ · 1.00
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Found its own results nicely agree with those of this paper at M<10^11 Msun but diverge at higher masses, though remaining consistent within the error bars.
The emergence of passive galaxies in the early Universe (2020) · 1.00 · paraphrased: the licence does not allow quoting
How the literature uses it
9 arXiv papers cite this in 28 sentences
Papers whose main result relates to this one's
States a conflicting result 1 paper
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Using an empirical correction to model the intrinsic GSMF, we find evidence for an evolving characteristic stellar mass with $\delta \log_{10}(M^*/M_\odot)/\delta z$ = $-0.16\pm0.05 \, (-0.11\pm0.05)$, when using SExtractor (ProFound).
Papers citing it · 12 sentences without a confident label
Contests it 1 paper
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[ref] 's $∼$9% implies the lowest $H$, but simulations show that these authors' UVJ passive selection—based on [ref] 's $z<0.5$ prescription—may miss 45% of intrinsically non-starforming galaxies at $z∼3$.[Tests assumed a Gaussian $A_V≤2$ mag distribution with a mean and dispersion of 0.5 mag, $logZ/Z_⊙=-0.5$, a [ref] initial mass function, and no photometric errors.
At Least One-in-Six Galaxies Is Always Dead · Introduction · contest 0.80
Uses its data or values 2 papers
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For the galaxy stellar mass function, we adopt a double Schechter function with empirical parameters given by [ref] .
Measuring cosmic expansion with diffractive gravitational scintillation of nanoHertz gravitational waves · Total integrated flux · 0.99
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By using current estimates of the galaxy stellar mass function for quenched and star forming galaxies ( [ref] , [ref] ), in Paper 2, we have found that $μ$ is likely to lie at intermediate values, $μ≈2.5$.
The size function of massive satellites from the $R_e-R_h$ and $M_{star}-M_h$ relations: constraining the role of environment · Methods · 0.93
Compares with it 3 papers
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For example [ref] , [ref] and [ref] find an approximately constant characteristic mass with redshift, but offset from each other by up to $M^* ∼0.5$dex.
Evolution of the galaxy stellar mass function: evidence for an increasing $M^*$ from $z=2$ to the present day · The evolution of the galaxy stellar mass function · 0.82
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We plot on Fig. [ref] the SMF of [ref] and [ref] , using the same redshift bins adopted by us, and the estimate of [ref] , covering a redshift space slightly larger than our first interval but equally centred at $z∼3.25$.
The emergence of passive galaxies in the early Universe · Comparison with previous observations · 0.99
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Because of the limited depth available for the SMFs of [ref] , we compare, in the right panel of Figure [ref], our measurements of the ratio of the stellar mass density and the dark matter halo density to those we obtain with the same procedure using the SMFs of [ref] and [ref] .
Galaxy Stellar Mass Functions from z~10 to z~6 using the Deepest Spitzer/IRAC Data: No Significant Evolution in the Stellar-to-Halo Mass Ratio of Galaxies in the First Gyr of Cosmic Time · Halo-mass density · 0.82
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