pith. sign in

arxiv: 2605.15893 · v1 · pith:2J53KRQCnew · submitted 2026-05-15 · 🌌 astro-ph.CO · astro-ph.GA· astro-ph.IM

Probing the faint-end of simulated galaxy counts at z>3

Flaminia Fortuni , Emiliano Merlin , Marco Castellano , Adriano Fontana , Paola Santini This is my paper

Pith reviewed 2026-05-20 18:43 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GAastro-ph.IM
keywords galaxy number countshigh-redshift galaxieshydrodynamical simulationsfaint-end luminosity functiongalaxy morphologyobservational completenessearly universe galaxy formationsurface brightness
0
0 comments X

The pith

Hydrodynamical simulations underproduce the faint compact galaxies seen in deep near-infrared observations at redshifts above 3.

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

The paper investigates a shortfall in the number of faint galaxies predicted by simulations compared to what is detected in deep fields at redshifts greater than 3. Through forward modeling of simulated galaxies into mock images that mimic real observations, it separates effects from detection limits and from the underlying galaxy formation physics. The analysis shows that while some diffuse galaxies are missed due to low surface brightness, the larger issue is that simulations produce too few compact galaxies with bright central cores. This matters because accurate counts of these faint sources are needed to understand the total light and mass buildup in the early universe. If the simulations are missing key physics, then current models of star formation and feedback require revision to match the observed populations.

Core claim

The discrepancy between observed and simulated faint-end galaxy counts at redshifts greater than 3 arises both from detection losses of diffuse galaxies and, more fundamentally, from the inability of current hydrodynamical simulations to produce enough faint compact galaxies. Forward modeling into mock images demonstrates that the deficit persists even after accounting for completeness and that increasing depth alone cannot resolve it, as simulations favor diffuse low-surface-brightness systems over the compact cores seen in data.

What carries the argument

Forward modeling of simulated lightcone catalogs into mock observational images to enable direct comparison of detected sources, which reveals systematic differences in galaxy structure between simulations and observations.

If this is right

  • The faint-end deficit appears consistently across different observational fields at redshifts above 3.
  • Structural analysis shows simulations produce more diffuse low-surface-brightness galaxies and fewer compact systems with bright cores.
  • Increasing the depth of mock images recovers counts near the completeness peak but overpredicts the faintest sources.
  • The tension indicates that adjustments to modeling of early star formation, feedback, and dust treatment are needed.

Where Pith is reading between the lines

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

  • The structural mismatch may require revisions to how galaxy sizes and concentrations are regulated in simulations at early times.
  • Resolving the count discrepancy could alter estimates of the total contribution from faint galaxies to the extragalactic background light.
  • Similar forward-modeling tests applied to other simulation suites could isolate whether the compact-galaxy deficit is widespread.

Load-bearing premise

The forward-modeling procedure and completeness corrections accurately capture all observational selection effects, allowing remaining differences to be attributed to simulation physics rather than unmodeled biases.

What would settle it

Deeper imaging that reveals a population of faint compact galaxies with bright central cores whose number and properties match the simulation predictions without overproducing the very faintest sources would challenge the conclusion that simulations fundamentally lack these objects.

Figures

Figures reproduced from arXiv: 2605.15893 by Adriano Fontana, Emiliano Merlin, Flaminia Fortuni, Marco Castellano, Paola Santini.

Figure 1
Figure 1. Figure 1: Number counts in the H band in the CANDELS fields (from left to right: COSMOS, EGS, UDS, GS, GSN). Both the mock detections (purple) and the IU counts (blue) are derived from the five cmd-TNG100 realizations; shaded areas indicate the 1σ scatter across the realizations. The mock images are simulated at the corresponding survey depth (i.e. at the 5σ limiting magnitude of the real datasets). Dashed colored l… view at source ↗
Figure 2
Figure 2. Figure 2: H band number counts divided into redshift bins (from top to bottom: z=0.0–2.9, z=3.0–3.6, and z=3.7–5.0). Left pan￾els show results from TNG100, right panels to EAGLE. Mock datasets, obtained from the five cmd- realizations, are repre￾sented by solid line with 1σ shaded area. The IU (blue for TNG100 and magenta for EAGLE) and the sources detected on the mock image (black for TNG100 and brown for EAGLE) ar… view at source ↗
Figure 4
Figure 4. Figure 4: Comparison between observed H-band number counts in the CANDELS GS field (dashed bright red) and IU counts from five cmd-TNG100 realizations (blue line with 1σ shaded area). The dashed dark red line shows the completeness￾corrected GS counts, obtained using the completeness curve at log10(Rhl/pix) = 0.6. Vertical lines indicate the 50% completeness magnitudes derived for different source sizes (log10(Rhl/p… view at source ↗
Figure 3
Figure 3. Figure 3: Completeness curves for fake sources injected into the [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of H-band number counts between the CAN￾DELS GS field (dashed red) and the FORECAST mock dataset based on five cmd-TNG100 realizations. Mock detections at GS depth are shown in black with 1σ shaded area, while the ‘deeper’ mock (cyan with shaded area) is obtained by reducing the noise by a factor of 10. IU counts are shown as the solid blue line. The dashed red line indicates GS counts corrected… view at source ↗
Figure 6
Figure 6. Figure 6: Characterization of the sources in GOODS-South (red) and in a mock image created from one of the [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Properties of galaxies at z > 3 detected in mock images with noise reduced by a factor of 10 relative to the nominal depth (‘deeper’ image; kept sources, violet/gray) and missed at nominal depth (lost, orange/pink). The upper panels show the intrinsic Input Universe properties of these galaxies: stellar mass, surface brightness within R = 3 pixels (µ3pix), FLUX_RADIUS_20 and FLUX_RADIUS_80, i.e. the radii … view at source ↗
read the original abstract

Simulations and observations now probe comparable redshift regimes with unprecedented accuracy, enabling direct consistency tests through forward modeling. In a previous work, we identified a faint-end discrepancy between observed and simulated near-infrared galaxy counts in CANDELS GOODS-South. Here we investigate whether this tension originates from the forward-modeling procedure or from limitations of the underlying simulations, and we characterize the galaxy populations responsible for the tension. Using the FORECAST forward modeling code, we generated ten independent lightcone realizations and mock CANDELS images from the TNG100 and EAGLE simulations. We compared both the intrinsic lightcone catalogs and the mock-image detections with observations, testing dependencies on field and redshift, and validating the pipeline through stellar mass and multi-band analyses. The faint-end deficit is present in all CANDELS fields and appears at z>3 in both simulations. GOODS-South counts corrected for completeness exceed intrinsic simulation counts already at the 50% completeness limit, indicating that the missing population is not simply hidden below the detection threshold. Increasing the depth of mock images recovers the counts near the peak but overpredicts the faintest sources, showing that depth alone cannot resolve the discrepancy. Structural analyses reveal that compact galaxies with bright central cores observed in GOODS-South are underproduced in simulations, which instead favor diffuse low-surface-brightness systems. We conclude that the discrepancy arises both from detection losses of diffuse galaxies and, more fundamentally, from the inability of current hydrodynamical simulations to produce enough faint compact galaxies at z>3. This tension points to the need for improved modeling of early star formation, feedback, and dust treatment.

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 forward-models TNG100 and EAGLE simulations into mock CANDELS images using the FORECAST code across ten independent lightcone realizations. It compares both intrinsic lightcone catalogs and mock detections to observational counts, finding a persistent faint-end deficit at z>3 that exceeds completeness-corrected observations already at the 50% limit and is attributed to underproduction of compact galaxies with bright cores in the simulations, alongside some detection losses of diffuse systems.

Significance. If the central claim holds, the work strengthens the case for limitations in current hydrodynamical simulations regarding early star formation, feedback, and dust at z>3, while demonstrating the value of multi-realization forward modeling for isolating simulation physics from observational selection. The reported field-to-field consistency and structural diagnostics provide a solid basis for the tension identified.

major comments (2)
  1. [completeness and detection analysis] § on completeness and detection (abstract and results): the claim that completeness-corrected CANDELS counts exceed intrinsic simulation counts at the 50% limit is load-bearing for ruling out simple threshold losses, but the manuscript provides limited detail on exact completeness modeling, error propagation, and how post-hoc choices in FORECAST affect the z>3 comparison; this needs explicit quantification to support attribution to simulation physics.
  2. [structural analyses] § on structural analyses: the distinction between observed compact galaxies and simulated diffuse systems assumes identical morphology measurement (e.g., concentration or core brightness) in mocks versus data. The abstract mentions validation via stellar mass and multi-band checks but does not detail how PSF, noise, background subtraction, or source-extraction thresholds are matched for different surface-brightness profiles; this is central to the claim that simulations underproduce faint compact galaxies.
minor comments (2)
  1. [methods] Clarify in the methods whether the ten lightcone realizations are fully independent or share initial conditions, and report the exact field-to-field variance in the counts.
  2. [results] The abstract states that increasing mock depth recovers counts near the peak but overpredicts the faintest sources; add a quantitative statement on the magnitude range where this transition occurs.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. The comments have identified areas where additional methodological detail will strengthen the presentation of our results. We address each major comment below and indicate the changes we will make in revision.

read point-by-point responses

  1. Referee: [completeness and detection analysis] § on completeness and detection (abstract and results): the claim that completeness-corrected CANDELS counts exceed intrinsic simulation counts at the 50% limit is load-bearing for ruling out simple threshold losses, but the manuscript provides limited detail on exact completeness modeling, error propagation, and how post-hoc choices in FORECAST affect the z>3 comparison; this needs explicit quantification to support attribution to simulation physics.

    Authors: We agree that explicit quantification of the completeness procedure is required to support the claim that the discrepancy is not due to simple detection threshold effects. In the revised manuscript we will expand the completeness and detection section to provide a full description of the modeling, including the precise algorithm used to compute completeness fractions, the propagation of Poisson and cosmic-variance uncertainties across the ten lightcone realizations, and the sensitivity of the z>3 comparison to the specific post-hoc choices made in FORECAST (e.g., source-extraction parameters and background estimation). We will include supplementary figures showing completeness curves versus magnitude for each field and redshift bin, together with the resulting corrected counts and their uncertainties at the 50% limit. revision: yes

  2. Referee: [structural analyses] § on structural analyses: the distinction between observed compact galaxies and simulated diffuse systems assumes identical morphology measurement (e.g., concentration or core brightness) in mocks versus data. The abstract mentions validation via stellar mass and multi-band checks but does not detail how PSF, noise, background subtraction, or source-extraction thresholds are matched for different surface-brightness profiles; this is central to the claim that simulations underproduce faint compact galaxies.

    Authors: We thank the referee for emphasizing the importance of demonstrating that morphological measurements are performed identically on mocks and data. The FORECAST pipeline convolves the simulated images with the CANDELS PSF, adds realistic noise, and applies the same background subtraction and source-extraction settings used on the observations. Nevertheless, we acknowledge that the current text does not provide sufficient detail on how these steps are tuned for galaxies with differing surface-brightness profiles. In revision we will add a dedicated subsection that (i) specifies the exact source-extraction thresholds and concentration/core-brightness definitions applied to both datasets, (ii) presents validation tests in which input mock morphologies are recovered after the full observational processing, and (iii) shows direct comparisons of the resulting structural-parameter distributions for the faint z>3 population. revision: yes

Circularity Check

0 steps flagged

No significant circularity; comparisons use external simulations and independent forward modeling.

full rationale

The paper generates mock CANDELS images from independent external simulations (TNG100 and EAGLE) via the FORECAST pipeline and directly compares intrinsic catalogs, detected counts, and structural properties to observational data. The central claim about missing faint compact galaxies follows from these count excesses (already at 50% completeness) and morphology differences, without any quantity being defined in terms of itself or a prediction forced by fitting the target dataset. The reference to prior work merely contextualizes the known discrepancy; the present analysis re-derives and extends the result across fields, depths, and structural metrics using new realizations. This keeps the chain self-contained against external benchmarks rather than reducing to self-citation or tautological input.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The claim rests on the fidelity of pre-existing hydrodynamical simulations and the accuracy of the FORECAST pipeline; no new free parameters, ad-hoc entities, or unstated mathematical axioms are introduced in this work.

axioms (1)
  • domain assumption The TNG100 and EAGLE simulations provide a sufficiently realistic representation of galaxy formation physics at z>3 for the purposes of this count comparison.
    The paper treats the simulation outputs as the baseline against which observations are compared.

pith-pipeline@v0.9.0 · 5838 in / 1450 out tokens · 68938 ms · 2026-05-20T18:43:17.670309+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

135 extracted references · 135 canonical work pages · 57 internal anchors

  1. [1]

    The EAGLE project: Simulating the evolution and assembly of galaxies and their environments

    The EAGLE project: simulating the evolution and assembly of galaxies and their environments. , keywords =. 2015. doi:10.1093/mnras/stu2058 , archivePrefix =. 1407.7040 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu2058 2015

  2. [2]

    , keywords =

    Hydrodynamical Simulations of the Galaxy Population: Enduring Successes and Outstanding Challenges. , keywords =. doi:10.1146/annurev-astro-041923-043618 , archivePrefix =. 2309.17075 , primaryClass =

    work page doi:10.1146/annurev-astro-041923-043618

  3. [3]

    The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations

    The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations. , keywords =. doi:10.1093/mnras/stv725 , archivePrefix =. 1501.01311 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv725

  4. [4]

    Supermassive black holes and their feedback effects in the IllustrisTNG simulation

    Supermassive black holes and their feedback effects in the IllustrisTNG simulation. , keywords =. 2018. doi:10.1093/mnras/sty1733 , archivePrefix =. 1710.04659 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1733 2018

  5. [5]

    Simulating Galaxy Formation with the IllustrisTNG Model

    Simulating galaxy formation with the IllustrisTNG model. , keywords =. 2018. doi:10.1093/mnras/stx2656 , archivePrefix =. 1703.02970 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx2656 2018

  6. [6]

    First results from the IllustrisTNG simulations: radio haloes and magnetic fields

    First results from the IllustrisTNG simulations: radio haloes and magnetic fields. , keywords =. doi:10.1093/mnras/sty2206 , archivePrefix =. 1707.03396 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2206

  7. [7]

    First results from the IllustrisTNG simulations: A tale of two elements -- chemical evolution of magnesium and europium

    First results from the IllustrisTNG simulations: a tale of two elements - chemical evolution of magnesium and europium. , keywords =. doi:10.1093/mnras/sty618 , archivePrefix =. 1707.03401 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty618

  8. [8]

    First results from the IllustrisTNG simulations: the galaxy color bimodality

    First results from the IllustrisTNG simulations: the galaxy colour bimodality. , keywords =. doi:10.1093/mnras/stx3040 , archivePrefix =. 1707.03395 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx3040

  9. [9]

    Monthly Notices of the Royal Astronomical Society , volume =

    Springel, Volker and Pakmor, Rüdiger and Pillepich, Annalisa and Weinberger, Rainer and Nelson, Dylan and Hernquist, Lars and Vogelsberger, Mark and Genel, Shy and Torrey, Paul and Marinacci, Federico and Naiman, Jill , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2017 , month =. doi:10.1093/mnras/stx3304 , url =

    work page doi:10.1093/mnras/stx3304 2017

  10. [10]

    Tidally Triggered Galaxy Formation. I. Evolution of the Galaxy Luminosity Function. , keywords =. doi:10.1086/170625 , adsurl =

    work page doi:10.1086/170625

  11. [11]

    , keywords =

    Galaxy Formation through Hierarchical Clustering. , keywords =. doi:10.1086/170483 , adsurl =

    work page doi:10.1086/170483

  12. [12]

    , keywords =

    Dynamics of Cooling Gas in Galactic Dark Halos. , keywords =. doi:10.1086/170590 , adsurl =

    work page doi:10.1086/170590

  13. [13]

    A Recipe for Galaxy Formation Shaun Cole

    A recipe for galaxy formation. , keywords =. doi:10.1093/mnras/271.4.781 , archivePrefix =. astro-ph/9402001 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/271.4.781

  14. [14]

    , eprint =

    Semi-analytic modelling of galaxy formation: the local Universe. , eprint =. doi:10.1046/j.1365-8711.1999.03032.x , adsurl =

    work page doi:10.1046/j.1365-8711.1999.03032.x 1999

  15. [15]

    , keywords =

    Hierarchical galaxy formation. , keywords =. doi:10.1046/j.1365-8711.2000.03879.x , archivePrefix =. astro-ph/0007281 , primaryClass =

    work page doi:10.1046/j.1365-8711.2000.03879.x 2000

  16. [16]

    The Physics of Galaxy Formation , year = "2001", editor =

    Semi-Analytical Models of Galaxy Formation. The Physics of Galaxy Formation , year = "2001", editor =

    work page 2001

  17. [17]

    A unified multi-wavelength model of galaxy formation

    A unified multiwavelength model of galaxy formation. , keywords =. doi:10.1093/mnras/stw1888 , archivePrefix =. 1509.08473 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw1888

  18. [18]

    Star Formation in Semi-Analytic Galaxy Formation Models with Multiphase Gas

    Star formation in semi-analytic galaxy formation models with multiphase gas. , keywords =. doi:10.1093/mnras/stv1877 , archivePrefix =. 1503.00755 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv1877

  19. [19]

    , keywords =

    Numerical techniques for large cosmological N-body simulations. , keywords =. doi:10.1086/191003 , adsurl =

    work page doi:10.1086/191003

  20. [20]

    , keywords =

    Stellar population synthesis at the resolution of 2003. , keywords =. doi:10.1046/j.1365-8711.2003.06897.x , archivePrefix =. astro-ph/0309134 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06897.x 2003

  21. [21]

    Modelling the nebular emission from primeval to present-day star-forming galaxies

    Modelling the nebular emission from primeval to present-day star-forming galaxies. , keywords =. doi:10.1093/mnras/stw1716 , archivePrefix =. 1607.06086 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw1716

  22. [22]

    Galactic Stellar and Substellar Initial Mass Function

    Galactic Stellar and Substellar Initial Mass Function. , keywords =. doi:10.1086/376392 , archivePrefix =. astro-ph/0304382 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/376392

  23. [23]

    The galaxy stellar mass function at 3.5<z<7.5 in the CANDELS/UDS, GOODS-South, and HUDF fields

    The galaxy stellar mass function at 3.5 z 7.5 in the CANDELS/UDS, GOODS-South, and HUDF fields. , keywords =. doi:10.1051/0004-6361/201424750 , archivePrefix =. 1412.0532 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201424750

  24. [24]

    The ASTRODEEP Frontier Fields catalogues. II. Photometric redshifts and rest frame properties in Abell-2744 and MACS-J0416. , keywords =. doi:10.1051/0004-6361/201527514 , archivePrefix =. 1603.02461 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201527514

  25. [25]

    CEERS Key Paper. I. An Early Look into the First 500 Myr of Galaxy Formation with JWST. , keywords =. doi:10.3847/2041-8213/acade4 , archivePrefix =. 2211.05792 , primaryClass =

    work page doi:10.3847/2041-8213/acade4 2041

  26. [26]

    , keywords =

    The Cosmic Evolution Early Release Science Survey (CEERS). , keywords =. doi:10.3847/2041-8213/adbbd3 , archivePrefix =. 2501.04085 , primaryClass =

    work page doi:10.3847/2041-8213/adbbd3 2041

  27. [27]

    CANDELS Multi-wavelength Catalogs: Source Detection and Photometry in the GOODS-South Field

    CANDELS Multi-wavelength Catalogs: Source Detection and Photometry in the GOODS-South Field. , keywords =. doi:10.1088/0067-0049/207/2/24 , archivePrefix =. 1308.4405 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/207/2/24

  28. [28]

    , keywords =

    The ASTRODEEP-GS43 catalogue: New photometry and redshifts for the CANDELS GOODS-South field. , keywords =. doi:10.1051/0004-6361/202140310 , archivePrefix =. 2103.09246 , primaryClass =

    work page doi:10.1051/0004-6361/202140310

  29. [29]

    , keywords =

    ASTRODEEP-JWST: NIRCam-HST multi-band photometry and redshifts for half a million sources in six extragalactic deep fields. , keywords =. doi:10.1051/0004-6361/202451409 , archivePrefix =. 2409.00169 , primaryClass =

    work page doi:10.1051/0004-6361/202451409

  30. [30]

    The Open Journal of Astrophysics , keywords =

    Witnessing downsizing in the making: quiescent and breathing galaxies at the dawn of the Universe. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.147267 , archivePrefix =. 2509.09764 , primaryClass =

    work page doi:10.33232/001c.147267

  31. [31]

    , keywords =

    FORECAST: A flexible software to forward model cosmological hydrodynamical simulations mimicking real observations. , keywords =. doi:10.1051/0004-6361/202346725 , archivePrefix =. 2305.19166 , primaryClass =

    work page doi:10.1051/0004-6361/202346725

  32. [32]

    , keywords =

    Mock galaxy surveys for HST and JWST from the IllustrisTNG simulations. , keywords =. doi:10.1093/mnras/stac3397 , archivePrefix =. 2211.09677 , primaryClass =

    work page doi:10.1093/mnras/stac3397

  33. [33]

    , keywords =

    SExtractor: Software for source extraction. , keywords =. doi:10.1051/aas:1996164 , adsurl =

    work page doi:10.1051/aas:1996164

  34. [34]

    Computational Astrophysics and Cosmology , keywords =

    The IllustrisTNG simulations: public data release. Computational Astrophysics and Cosmology , keywords =. doi:10.1186/s40668-019-0028-x , archivePrefix =. 1812.05609 , primaryClass =

    work page doi:10.1186/s40668-019-0028-x

  35. [35]

    First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies

    First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies. , keywords =. doi:10.1093/mnras/stx3112 , archivePrefix =. 1707.03406 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx3112

  36. [36]

    CANDELS Multiwavelength catalogs: Source Identification and Photometry in the CANDELS UKIDSS Ultra-Deep Survey Field

    CANDELS Multiwavelength Catalogs: Source Identification and Photometry in the CANDELS UKIDSS Ultra-deep Survey Field. , keywords =. doi:10.1088/0067-0049/206/2/10 , archivePrefix =. 1305.1823 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/206/2/10

  37. [37]

    Chasing passive galaxies in the early Universe: a critical analysis in CANDELS GOODS-South

    Chasing passive galaxies in the early Universe: a critical analysis in CANDELS GOODS-South. , keywords =. doi:10.1093/mnras/stx2385 , archivePrefix =. 1709.00429 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx2385

  38. [38]

    CANDELS: The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey

    CANDELS: The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. , keywords =. doi:10.1088/0067-0049/197/2/35 , archivePrefix =. 1105.3753 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/197/2/35

  39. [39]

    CANDELS: The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey - The Hubble Space Telescope Observations, Imaging Data Products and Mosaics

    CANDELS: The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey The Hubble Space Telescope Observations, Imaging Data Products, and Mosaics. , keywords =. doi:10.1088/0067-0049/197/2/36 , archivePrefix =. 1105.3754 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/197/2/36

  40. [40]

    Horizon-AGN virtual observatory - 1. SED-fitting performance and forecasts for future imaging surveys

    Horizon-AGN virtual observatory - 1. SED-fitting performance and forecasts for future imaging surveys. , keywords =. doi:10.1093/mnras/stz1054 , archivePrefix =. 1903.10934 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1054 1903

  41. [41]

    , keywords =

    Deep Realistic Extragalactic Model (DREaM) Galaxy Catalogs: Predictions for a Roman Ultra-deep Field. , keywords =. doi:10.3847/1538-4357/ac46fb , archivePrefix =. 2110.10703 , primaryClass =

    work page doi:10.3847/1538-4357/ac46fb

  42. [42]

    , keywords =

    The BLUETIDES mock image catalogue: simulated observations of high-redshift galaxies and predictions for JWST imaging surveys. , keywords =. doi:10.1093/mnras/stac2111 , archivePrefix =. 2206.08941 , primaryClass =

    work page doi:10.1093/mnras/stac2111

  43. [43]

    , keywords =

    Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations. , keywords =. doi:10.1093/mnras/staa4043 , archivePrefix =. 2006.15156 , primaryClass =

    work page doi:10.1093/mnras/staa4043 2006

  44. [44]

    , keywords =

    MOCK OBSERVATORY: Two thousand light-cone mock catalogues of luminous red galaxies from the Hyper Suprime-Cam Survey for the cosmological large-scale analysis. , keywords =. doi:10.1093/mnras/stae648 , archivePrefix =. 2308.03871 , primaryClass =

    work page doi:10.1093/mnras/stae648

  45. [45]

    The Hyper Suprime-Cam SSP Survey: Overview and Survey Design

    The Hyper Suprime-Cam SSP Survey: Overview and survey design. , keywords =. doi:10.1093/pasj/psx066 , archivePrefix =. 1704.05858 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/pasj/psx066

  46. [46]

    , keywords =

    The impact of AGN-driven winds on physical and observable galaxy sizes. , keywords =. doi:10.1093/mnras/stad1528 , archivePrefix =. 2303.12858 , primaryClass =

    work page doi:10.1093/mnras/stad1528

  47. [47]

    , keywords =

    Disappearing Galaxies: The Orientation Dependence of JWST-bright, HST-dark, Star-forming Galaxy Selection. , keywords =. doi:10.3847/1538-4357/ad02f8 , archivePrefix =. 2310.08829 , primaryClass =

    work page doi:10.3847/1538-4357/ad02f8

  48. [48]

    iMaNGA: mock MaNGA galaxies based on IllustrisTNG and MaStar SSPs. - III. Stellar metallicity drivers in MaNGA and TNG50. , keywords =. doi:10.1093/mnras/stad3599 , archivePrefix =. 2309.14257 , primaryClass =

    work page doi:10.1093/mnras/stad3599

  49. [49]

    , keywords =

    Secondary standard stars for absolute spectrophotometry. , keywords =. doi:10.1086/160817 , adsurl =

    work page doi:10.1086/160817

  50. [50]

    Evolution of galaxy stellar masses and star formation rates in the EAGLE simulations

    Evolution of galaxy stellar masses and star formation rates in the EAGLE simulations. , keywords =. doi:10.1093/mnras/stv852 , archivePrefix =. 1410.3485 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv852

  51. [51]

    The EAGLE simulations of galaxy formation: Public release of particle data

    The EAGLE simulations of galaxy formation: Public release of particle data. arXiv e-prints , keywords =. doi:10.48550/arXiv.1706.09899 , archivePrefix =. 1706.09899 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1706.09899

  52. [52]

    Dancing in the dark: galactic properties trace spin swings along the cosmic web

    Dancing in the dark: galactic properties trace spin swings along the cosmic web. , keywords =. doi:10.1093/mnras/stu1227 , archivePrefix =. 1402.1165 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu1227

  53. [53]

    , keywords =

    Introducing the NEWHORIZON simulation: Galaxy properties with resolved internal dynamics across cosmic time. , keywords =. doi:10.1051/0004-6361/202039429 , archivePrefix =. 2009.10578 , primaryClass =

    work page doi:10.1051/0004-6361/202039429 2009

  54. [54]

    Simba: Cosmological Simulations with Black Hole Growth and Feedback

    SIMBA: Cosmological simulations with black hole growth and feedback. , keywords =. doi:10.1093/mnras/stz937 , archivePrefix =. 1901.10203 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz937 1901

  55. [55]

    , keywords =

    The FLAMINGO project: cosmological hydrodynamical simulations for large-scale structure and galaxy cluster surveys. , keywords =. doi:10.1093/mnras/stad2419 , archivePrefix =. 2306.04024 , primaryClass =

    work page doi:10.1093/mnras/stad2419

  56. [56]

    , keywords =

    The MillenniumTNG Project: the hydrodynamical full physics simulation and a first look at its galaxy clusters. , keywords =. doi:10.1093/mnras/stac3620 , archivePrefix =. 2210.10060 , primaryClass =

    work page doi:10.1093/mnras/stac3620

  57. [57]

    , keywords =

    Introducing the THESAN project: radiation-magnetohydrodynamic simulations of the epoch of reionization. , keywords =. doi:10.1093/mnras/stab3710 , archivePrefix =. 2110.00584 , primaryClass =

    work page doi:10.1093/mnras/stab3710

  58. [58]

    , keywords =

    The ASTRID simulation: galaxy formation and reionization. , keywords =. doi:10.1093/mnras/stac648 , archivePrefix =. 2111.01160 , primaryClass =

    work page doi:10.1093/mnras/stac648

  59. [59]

    , keywords =

    High-redshift JWST predictions from IllustrisTNG: dust modelling and galaxy luminosity functions. , keywords =. doi:10.1093/mnras/staa137 , archivePrefix =. 1904.07238 , primaryClass =

    work page doi:10.1093/mnras/staa137 1904

  60. [60]

    , keywords =

    Infrared luminosity functions and dust mass functions in the EAGLE simulation. , keywords =. doi:10.1093/mnras/staa990 , archivePrefix =. 2004.02713 , primaryClass =

    work page doi:10.1093/mnras/staa990 2004

  61. [61]

    Colours and luminosities of z=0.1 simulated galaxies in the EAGLE simulations

    Colours and luminosities of z = 0.1 galaxies in the EAGLE simulation. , keywords =. doi:10.1093/mnras/stv1461 , archivePrefix =. 1504.04374 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv1461

  62. [62]

    Infrared luminosity functions, obscured star formation, and dust temperature of high-redshift galaxies

    High-redshift predictions from IllustrisTNG - III. Infrared luminosity functions, obscured star formation, and dust temperature of high-redshift galaxies. , keywords =. doi:10.1093/mnras/stab3794 , archivePrefix =. 2104.12788 , primaryClass =

    work page doi:10.1093/mnras/stab3794

  63. [63]

    Planck 2013 results. I. Overview of products and scientific results. , keywords =. doi:10.1051/0004-6361/201321529 , archivePrefix =. 1303.5062 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201321529 2013

  64. [64]

    Results at z=0

    Populating a cluster of galaxies - I. Results at z=0. , keywords =. doi:10.1046/j.1365-8711.2001.04912.x , archivePrefix =. astro-ph/0012055 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.04912.x 2001

  65. [65]

    , keywords =

    Substructures in hydrodynamical cluster simulations. , keywords =. doi:10.1111/j.1365-2966.2009.15034.x , archivePrefix =. 0808.3401 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15034.x 2009

  66. [66]

    , keywords =

    The cosmological simulation code GADGET-2. , keywords =. doi:10.1111/j.1365-2966.2005.09655.x , archivePrefix =. astro-ph/0505010 , primaryClass =

    work page doi:10.1111/j.1365-2966.2005.09655.x 2005

  67. [67]

    , keywords =

    E pur si muove: Galilean-invariant cosmological hydrodynamical simulations on a moving mesh. , keywords =. doi:10.1111/j.1365-2966.2009.15715.x , archivePrefix =. 0901.4107 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15715.x 2009

  68. [68]

    Planck 2015 results. I. Overview of products and scientific results. , keywords =. doi:10.1051/0004-6361/201527101 , archivePrefix =. 1502.01582 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201527101 2015

  69. [69]

    , keywords =

    On the relation between the Schmidt and Kennicutt-Schmidt star formation laws and its implications for numerical simulations. , keywords =. doi:10.1111/j.1365-2966.2007.12639.x , archivePrefix =. 0709.0292 , primaryClass =

    work page doi:10.1111/j.1365-2966.2007.12639.x 2007

  70. [70]

    , author Tavecchio, F

    Simulating galactic outflows with thermal supernova feedback. , keywords =. doi:10.1111/j.1365-2966.2012.21704.x , archivePrefix =. 1203.5667 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.21704.x 2012

  71. [71]

    , keywords =

    Cosmological simulations of the growth of supermassive black holes and feedback from active galactic nuclei: method and tests. , keywords =. doi:10.1111/j.1365-2966.2009.15043.x , archivePrefix =. 0904.2572 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15043.x 2009

  72. [72]

    , keywords =

    Cosmological smoothed particle hydrodynamics simulations: a hybrid multiphase model for star formation. , keywords =. doi:10.1046/j.1365-8711.2003.06206.x , archivePrefix =. astro-ph/0206393 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06206.x 2003

  73. [73]

    Simulations of magnetic fields in isolated disk galaxies

    Simulations of magnetic fields in isolated disc galaxies. , keywords =. doi:10.1093/mnras/stt428 , archivePrefix =. 1212.1452 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt428

  74. [74]

    A physical model for cosmological simulations of galaxy formation: multi-epoch validation

    A model for cosmological simulations of galaxy formation physics: multi-epoch validation. , keywords =. doi:10.1093/mnras/stt2295 , archivePrefix =. 1305.4931 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt2295

  75. [75]

    , keywords =

    The emergence of passive galaxies in the early Universe. , keywords =. doi:10.1051/0004-6361/202039738 , archivePrefix =. 2011.10584 , primaryClass =

    work page doi:10.1051/0004-6361/202039738 2011

  76. [76]

    , keywords =

    Red and dead CANDELS: massive passive galaxies at the dawn of the Universe. , keywords =. doi:10.1093/mnras/stz2615 , archivePrefix =. 1909.07996 , primaryClass =

    work page doi:10.1093/mnras/stz2615 1909

  77. [77]

    Introducing the Illustris Project: the evolution of galaxy populations across cosmic time

    Introducing the Illustris project: the evolution of galaxy populations across cosmic time. , keywords =. doi:10.1093/mnras/stu1654 , archivePrefix =. 1405.3749 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu1654

  78. [78]

    Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe

    Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe. , keywords =. doi:10.1093/mnras/stu1536 , archivePrefix =. 1405.2921 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu1536

  79. [79]

    The Illustris simulation: the evolving population of black holes across cosmic time

    The Illustris simulation: the evolving population of black holes across cosmic time. , keywords =. doi:10.1093/mnras/stv1340 , archivePrefix =. 1408.6842 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv1340

  80. [80]

    , keywords =

    The baryon cycle in modern cosmological hydrodynamical simulations. , keywords =. doi:10.1093/mnras/stae1688 , archivePrefix =. 2402.08408 , primaryClass =

    work page doi:10.1093/mnras/stae1688

Showing first 80 references.