pith. sign in

arxiv: 2606.31628 · v1 · pith:5VB2EOGKnew · submitted 2026-06-30 · 🌌 astro-ph.GA

A big step forward with SHARP: spatially resolved stellar population properties in passive galaxies at z > 1.5

A. Gargiulo , C. Mancini , F. R. Ditrani , S. Bisogni , P. Franzetti , G. Vietri , A. Gallazzi , M. Longhetti
show 1 more author
S. Zibetti
This is my paper

Pith reviewed 2026-07-01 04:34 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galaxy evolutionquiescent galaxiesstellar populationsintegral field spectroscopyhigh-redshift galaxiesELT instrumentsCOSMOS surveystellar gradients
0
0 comments X

The pith

SHARP at the ELT can map stellar population gradients out to 2Re in most massive quiescent galaxies at z < 2.5 with 20-hour exposures.

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

The paper conducts a feasibility study for the proposed SHARP/VESPER integral field unit on the Extremely Large Telescope to obtain spatially resolved measurements of stellar age, metallicity, and enrichment in passive galaxies at redshifts 1.5 to 3. It selects a sample of massive quiescent systems from the COSMOS-Web catalogue, models them as compact and extended galaxies, and runs simulations through the official SHARP exposure time calculator to determine the integration times needed for signal-to-noise ratios of 10-15 per resolution element. The results indicate that routine mapping to twice the effective radius becomes practical for the majority of such galaxies below redshift 2.5 in roughly 20 hours, while redshift 3 targets reach at least one effective radius in about 30 hours. This setup would also resolve the central kiloparsec at all considered redshifts, permitting direct checks on whether central mass buildup drives quenching.

Core claim

Using the COSMOS-Web catalogue to define a realistic population of massive quiescent galaxies at 1.5 < z < 3 and modeling representative compact and extended systems, simulations with the SHARP ETC show that exposure times of about 20 hours suffice to reach S/N = 10-15 per resolution element out to 2Re for the majority at z < 2.5, while 30 hours reach at least Re at z = 3. The 30 mas resolution enabled by MORFEO MCAO resolves the inner < 1 kpc at all redshifts, allowing direct tests of quenching mechanisms tied to central mass build-up, bulge growth, and structural transformation.

What carries the argument

Simulations with the official SHARP exposure time calculator applied to compact and extended galaxy models drawn from the COSMOS-Web catalogue.

If this is right

  • Stellar population gradients become measurable out to 2Re for most massive quiescent galaxies at z < 2.5 in integrations of about 20 hours.
  • At z = 3 the same measurements reach at least Re with about 30 hours of integration.
  • The inner < 1 kpc region is resolved at all redshifts considered, enabling tests of quenching linked to central mass build-up.
  • Statistically meaningful, spatially resolved stellar population constraints become available during the epoch when stellar cores of these galaxies were assembled.

Where Pith is reading between the lines

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

  • Such maps could be combined with lower-redshift samples to trace how radial age and metallicity patterns evolve over cosmic time.
  • The ability to resolve central regions might distinguish between quenching scenarios that predict different inner stellar population signatures.
  • The exposure time estimates provide a benchmark that could guide observing strategies for similar IFU instruments on other large telescopes.

Load-bearing premise

The COSMOS-Web catalogue supplies a representative sample of massive quiescent galaxies at 1.5 < z < 3 and the chosen compact and extended structural models accurately capture the properties that determine required exposure times.

What would settle it

On-sky SHARP observations that require substantially more than 30 hours to reach S/N = 10-15 at z = 3 or fail to resolve structures inside 1 kpc as predicted by the models.

Figures

Figures reproduced from arXiv: 2606.31628 by A. Gallazzi, A. Gargiulo, C. Mancini, F. R. Ditrani, G. Vietri, M. Longhetti, P. Franzetti, S. Bisogni, S. Zibetti.

Figure 1
Figure 1. Figure 1: NUV–𝑟–J colour–colour diagram for the massive passive sample in four redshift bins. Circle and star points show all galaxies with log(𝑀⋆∕𝑀⊙) > 10.5 and log(sSFR∕yr−1) < −10. Red lines indicate the passive selection criteria of Ilbert et al. (2013). Circle symbols highlight galaxies satisfying both the sSFR and colour-based selections. The colour scale traces the sSFR. distribution of galaxies at higher red… view at source ↗
Figure 2
Figure 2. Figure 2: F150W magnitude distribution of the massive passive sample in four redshift bins (solid blue lines). The pale-blue shaded histogram shows the distribution of galaxies with log(𝑀⋆∕𝑀⊙) > 11. In each panel, solid(dashed) line indicates the 80th-pecentile of the distribution for the full(most massive) sample [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Effective radius versus F150W magnitude in four redshift bins. Pale-blue open circles show the full massive passive sample; filled symbols highlight galaxies with log(𝑀⋆∕𝑀⊙) > 11. The dashed lines in the 3 ≤ 𝑧 < 4 panel mark an illustrative region (H < 24 and 𝑅e < 0.15′′) corresponding to one of the size–magnitude combinations for which SHARP is expected to reach 𝑆∕𝑁 levels suitable for measuring stellar p… view at source ↗
Figure 4
Figure 4. Figure 4: Redshifted spectra of a 2 Gyr single stellar population template (solar metallicity, Bruzual & Charlot, 2016) shown at 𝑧 = 1.5, 𝑧 = 2, 𝑧 = 2.5, and 𝑧 = 3 (from top to bottom). The strong continuum slopes characteristic of passive galaxies at these epochs are clearly visible. The vertical dashed lines mark the two reference wavelengths, 𝜆 = 1.5 𝜇m and 𝜆 = 2.2 𝜇m, at which the 𝑆∕𝑁 estimates discussed in Sect… view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of different stellar population models used to test the robustness of our ETC results. The blue curve shows the reference simple stellar population (SSP) with age 2 Gyr and solar metallicity adopted throughout this work. The green curve represents an SSP with the same age but lower metallicity (20% Z⊙), while the magenta curve shows a composite stellar population (CSP) with an exponentially decl… view at source ↗
read the original abstract

Understanding when and how massive quiescent galaxies (log(M*/Msun) > 10.5) assembled their stellar mass and quenched remains a central challenge in galaxy evolution. Spatially resolved stellar population measurements at z > 1.5 offer a uniquely powerful avenue to address this problem, as they can provide information on the radial variations in stellar age, metallicity, and enrichment histories in passive galaxies as they first emerge. In this work, we present a feasibility study quantifying the transformative capabilities of the proposed IFU SHARP/VESPER at the ELT for performing such radial mapping of stellar population gradients in passive galaxies at 1.5 < z < 3. Using the COSMOS-Web catalogue, we define a realistic population of massive quiescent systems at 1.5 < z < 3 and model representative compact and extended galaxies across this redshift range. Through detailed simulations with the official SHARP ETC, we derive the exposure times required to reach S/N = 10-15 per resolution element at key rest-frame optical wavelengths. Our results show that SHARP will routinely measure stellar population gradients out to 2Re for the majority of the population at z < 2.5 with integrations of about 20h, and that will reach at least Re in about 30h at z = 3. Thanks to MORFEO's MCAO and to its spatial resolution of 30mas SHARP/VESPER will also resolve the inner < 1kpc at all redshifts considered, enabling for the first time, direct tests of quenching mechanisms linked to central mass build-up, bulge growth, and structural transformation. These findings demonstrate that SHARP/VESPER will open an entirely new observational window on the early evolution of massive quiescent galaxies, providing, for the first time, statistically meaningful, spatially resolved stellar population constraints during the epoch when their stellar cores were assembled.

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

1 major / 1 minor

Summary. The manuscript is a feasibility study for the proposed SHARP/VESPER IFU on the ELT, using the COSMOS-Web catalogue to select massive quiescent galaxies at 1.5 < z < 3, modeling representative compact and extended systems, and running the official SHARP ETC to compute exposure times for S/N = 10-15 per resolution element at rest-frame optical wavelengths. It concludes that ~20 h integrations enable stellar population gradient measurements out to 2Re for the majority of the population at z < 2.5, while ~30 h reach at least Re at z = 3, with the MCAO resolution also resolving the inner <1 kpc at all redshifts.

Significance. If the exposure-time projections hold, the result would be significant because it quantifies how SHARP/VESPER can deliver the first statistically meaningful, spatially resolved stellar population constraints on massive quiescent galaxies during the epoch of core assembly, directly testing quenching mechanisms tied to central mass build-up and structural transformation. The use of an external catalog for sample definition and the official ETC for forward modeling are strengths that make the projections more reproducible.

major comments (1)
  1. [Abstract (sample definition and modeling paragraph)] Abstract (sample definition and modeling paragraph): the headline exposure times (20 h to 2Re at z < 2.5; 30 h to Re at z = 3) are obtained by feeding COSMOS-Web-derived compact/extended structural models into the SHARP ETC and requiring S/N = 10-15 per resolution element. No sensitivity analysis to plausible variations in Re, Sersic index, or surface-brightness profile is presented; any systematic offset toward lower surface brightness would increase the quoted times, making this assumption load-bearing for the central claim.
minor comments (1)
  1. Clarify in the methods section the precise quantitative criteria used to define the 'representative compact and extended' models (e.g., ranges in Re, n, and magnitude) so that readers can assess how the chosen parameters map onto the COSMOS-Web parent sample.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments on our manuscript. We address the major comment below.

read point-by-point responses

  1. Referee: [Abstract (sample definition and modeling paragraph)] Abstract (sample definition and modeling paragraph): the headline exposure times (20 h to 2Re at z < 2.5; 30 h to Re at z = 3) are obtained by feeding COSMOS-Web-derived compact/extended structural models into the SHARP ETC and requiring S/N = 10-15 per resolution element. No sensitivity analysis to plausible variations in Re, Sersic index, or surface-brightness profile is presented; any systematic offset toward lower surface brightness would increase the quoted times, making this assumption load-bearing for the central claim.

    Authors: We agree that this is a valid point and that the headline exposure times rest on the adopted structural parameters. Our analysis employs representative compact and extended models drawn directly from the COSMOS-Web catalogue to reflect the observed population, but we did not explore variations in Re, Sersic index or surface-brightness profile. In the revised manuscript we will add a dedicated sensitivity analysis (new subsection or appendix) that perturbs these parameters across the observed ranges at 1.5 < z < 3 and quantifies the resulting changes in required integration time. This will demonstrate the robustness of the quoted 20 h and 30 h figures. revision: yes

Circularity Check

0 steps flagged

No circularity: forward projections from external catalog and instrument ETC

full rationale

The paper's central claims are exposure-time estimates obtained by selecting galaxies from the independent COSMOS-Web catalog, adopting representative structural models, and feeding them into the official SHARP ETC to compute required integrations for target S/N. No equations, parameters, or results are defined in terms of the output quantities themselves, no self-citations underpin the load-bearing steps, and no fitted inputs are relabeled as predictions. The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard assumptions about galaxy structural models and instrument performance that are not independently validated within the paper; no free parameters are fitted to new data and no new entities are postulated.

axioms (2)
  • domain assumption COSMOS-Web catalogue provides a representative sample of massive quiescent galaxies at 1.5<z<3
    Invoked when defining the realistic population for simulations (abstract).
  • domain assumption Compact and extended structural models accurately represent the population properties that set exposure times
    Used to model representative galaxies across the redshift range (abstract).

pith-pipeline@v0.9.1-grok · 5928 in / 1493 out tokens · 44334 ms · 2026-07-01T04:34:37.647898+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

45 extracted references · 45 canonical work pages · 19 internal anchors

  1. [1]

    Cheng, C. M. and et al. , title = ". MNRAS , keywords =. doi:10.1093/mnras/stae1739 , archivePrefix =. 2407.10974 , primaryClass =

    work page doi:10.1093/mnras/stae1739

  2. [2]

    On the Restricted Isometry Property of Centered Self Khatri-Rao Products

    Stellar Population Diagnostics of Elliptical Galaxy Formation. ARA & A , keywords =. doi:10.1146/annurev.astro.44.051905.092450 , archivePrefix =. astro-ph/0603479 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev.astro.44.051905.092450

  3. [3]

    T., Tanvir, N

    Environment and self-regulation in galaxy formation. MNRAS , keywords =. doi:10.1111/j.1365-2966.2010.16427.x , archivePrefix =. 0912.0259 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.16427.x 2010

  4. [4]

    MNRAS , keywords =

    Insights into formation scenarios of massive early-type galaxies from spatially resolved stellar population analysis in CALIFA. MNRAS , keywords =. doi:10.1093/mnras/stz3205 , archivePrefix =. 1906.02209 , primaryClass =

    work page doi:10.1093/mnras/stz3205 1906

  5. [5]

    The VLT LEGA-C Spectroscopic Survey: The Physics of Galaxies at a Lookback Time of 7 Gyr

    The VLT LEGA-C Spectroscopic Survey: The Physics of Galaxies at a Lookback Time of 7 Gyr. APJS , keywords =. doi:10.3847/0067-0049/223/2/29 , archivePrefix =. 1603.05479 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0067-0049/223/2/29

  6. [6]

    MNRAS , keywords =

    Inverse stellar population age gradients of post-starburst galaxies at z = 0.8 with LEGA-C. MNRAS , keywords =. doi:10.1093/mnras/staa1937 , archivePrefix =. 2007.00663 , primaryClass =

    work page doi:10.1093/mnras/staa1937 2007

  7. [7]

    VIMOS Public Extragalactic Redshift Survey (VIPERS). The distinct build-up of dense and normal massive passive galaxies

    The VIMOS Public Extragalactic Redshift Survey (VIPERS). The distinct build-up of dense and normal massive passive galaxies. AAP , keywords =. doi:10.1051/0004-6361/201630112 , archivePrefix =. 1611.07047 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201630112

  8. [8]

    3D-HST+CANDELS: The Evolution of the Galaxy Size-Mass Distribution since $z=3$

    3D-HST+CANDELS: The Evolution of the Galaxy Size-Mass Distribution since z = 3. APJ , keywords =. doi:10.1088/0004-637X/788/1/28 , archivePrefix =. 1404.2844 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/788/1/28

  9. [9]

    A., Primack, J

    The Kormendy relation of massive elliptical galaxies at z -0.5ex 1.5: evidence for size evolution. MNRAS , keywords =. doi:10.1111/j.1365-2966.2006.11171.x , archivePrefix =. astro-ph/0610241 , primaryClass =

    work page doi:10.1111/j.1365-2966.2006.11171.x 2006

  10. [10]

    Passively Evolving Early-type Galaxies at 1.4<z<2.5 in the Hubble Ultra Deep Field

    Passively Evolving Early-Type Galaxies at 1.4 < -0.5ex z < -0.5ex 2.5 in the Hubble Ultra Deep Field. ApJ , keywords =. doi:10.1086/430104 , archivePrefix =. astro-ph/0503102 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/430104

  11. [11]

    , keywords =

    SPIDER - VII. Revealing the stellar population content of massive early-type galaxies out to 8R _ e. MNRAS , keywords =. doi:10.1111/j.1365-2966.2012.21848.x , archivePrefix =. 1208.0587 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.21848.x 2012

  12. [12]

    T., Tanvir, N

    Early-type galaxies at large galactocentric radii - II. Metallicity gradients and the [Z/H]-mass, [ /Fe]-mass relations. MNRAS , keywords =. doi:10.1111/j.1365-2966.2010.17080.x , archivePrefix =. 1006.1698 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17080.x 2010

  13. [13]

    SDSS-IV MaNGA: stellar population gradients as a function of galaxy environment

    SDSS-IV MaNGA: stellar population gradients as a function of galaxy environment. MNRAS , keywords =. doi:10.1093/mnras/stw2719 , archivePrefix =. 1612.01545 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2719

  14. [14]

    The CALIFA survey across the Hubble sequence: Spatially resolved stellar population properties in galaxies

    The CALIFA survey across the Hubble sequence. Spatially resolved stellar population properties in galaxies. AAP , keywords =. doi:10.1051/0004-6361/201525938 , archivePrefix =. 1506.04157 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201525938

  15. [15]

    , keywords =

    GRAPE-SPH chemodynamical simulation of elliptical galaxies - I. Evolution of metallicity gradients. MNRAS , keywords =. doi:10.1111/j.1365-2966.2004.07258.x , archivePrefix =. astro-ph/0310160 , primaryClass =

    work page doi:10.1111/j.1365-2966.2004.07258.x 2004

  16. [16]

    On the survival of metallicity gradients to major dry-mergers

    On the survival of metallicity gradients to major dry-mergers. AAP , keywords =. doi:10.1051/0004-6361/200911715 , archivePrefix =. 0903.2846 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200911715

  17. [17]

    The stellar accretion origin of stellar population gradients in massive galaxies at large radii

    The stellar accretion origin of stellar population gradients in massive galaxies at large radii. MNRAS , keywords =. doi:10.1093/mnras/stv274 , archivePrefix =. 1410.2244 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv274

  18. [18]

    ApJL , keywords =

    Rest-frame Near-infrared Sizes of Galaxies at Cosmic Noon: Objects in JWST's Mirror Are Smaller than They Appeared. ApJL , keywords =. doi:10.3847/2041-8213/ac8e06 , archivePrefix =. 2207.10655 , primaryClass =

    work page doi:10.3847/2041-8213/ac8e06 2041

  19. [19]

    APJ , keywords =

    Medium Bands, Mega Science: A JWST/NIRCam Medium-band Imaging Survey of A2744. APJ , keywords =. doi:10.3847/1538-4357/ad75fe , archivePrefix =. 2404.13132 , primaryClass =

    work page doi:10.3847/1538-4357/ad75fe

  20. [20]

    MNRAS , keywords =

    A surprising abundance of massive quiescent galaxies at 3 < z < 5 in the first data from JWST CEERS. MNRAS , keywords =. doi:10.1093/mnras/stad369 , archivePrefix =. 2208.00986 , primaryClass =

    work page doi:10.1093/mnras/stad369

  21. [21]

    Nature , keywords =

    A massive quiescent galaxy at redshift 4.658. Nature , keywords =. doi:10.1038/s41586-023-06158-6 , archivePrefix =. 2301.11413 , primaryClass =

    work page doi:10.1038/s41586-023-06158-6

  22. [22]

    Half-mass radii for ~7,000 galaxies at 1.0 < z < 2.5: most of the evolution in the mass-size relation is due to color gradients

    Half-mass Radii for 7000 Galaxies at 1.0 z 2.5: Most of the Evolution in the Mass-Size Relation Is Due to Color Gradients. APJ , keywords =. doi:10.3847/1538-4357/ab1bda , archivePrefix =. 1904.10992 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab1bda 1904

  23. [23]

    , keywords =

    Spatially resolved colours and stellar population properties in early-type galaxies at z 1.5. MNRAS , keywords =. doi:10.1111/j.1365-2966.2012.21670.x , archivePrefix =. 1207.2295 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.21670.x 2012

  24. [24]

    ApJL , keywords =

    Remarkably Compact Quiescent Candidates at 3 < z < 5 in JWST-CEERS. ApJL , keywords =. doi:10.3847/2041-8213/ad2b6d , archivePrefix =. 2311.05394 , primaryClass =

    work page doi:10.3847/2041-8213/ad2b6d 2041

  25. [25]

    APJ , keywords =

    REQUIEM-2D: A Diversity of Formation Pathways in a Sample of Spatially Resolved Massive Quiescent Galaxies at z 2. APJ , keywords =. doi:10.3847/1538-4357/aca677 , archivePrefix =. 2203.04979 , primaryClass =

    work page doi:10.3847/1538-4357/aca677

  26. [26]

    AAP , keywords =

    Stellar population gradients at cosmic noon as a constraint to the evolution of passive galaxies. AAP , keywords =. doi:10.1051/0004-6361/202142523 , archivePrefix =. 2202.04086 , primaryClass =

    work page doi:10.1051/0004-6361/202142523

  27. [27]

    ApJL , keywords =

    Resolved Multi-element Stellar Chemical Abundances in the Brightest Quiescent Galaxy at z 2. ApJL , keywords =. doi:10.3847/2041-8213/aba11c , archivePrefix =. 2007.00205 , primaryClass =

    work page doi:10.3847/2041-8213/aba11c 2041

  28. [28]

    Clues to inside-out quenching in quiescent galaxies at $1.2\lesssim z\lesssim2.2$: Age, Fe-, and Mg-abundance gradients from JWST-SUSPENSE

    Building up JWST-SUSPENSE: inside-out quenching at cosmic noon from age, Fe-, and Mg-abundance gradients. arXiv e-prints , keywords =. doi:10.48550/arXiv.2509.12316 , archivePrefix =. 2509.12316 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2509.12316

  29. [29]

    T., Zhang, B., et al

    High-redshift elliptical galaxies: are they (all) really compact?. MNRAS , keywords =. doi:10.1111/j.1365-2966.2009.15728.x , archivePrefix =. 0909.3088 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15728.x 2009

  30. [30]

    MNRAS , keywords =

    The number density of superdense early-type galaxies at 1 < z < 2 and the local cluster galaxies. MNRAS , keywords =. doi:10.1111/j.1745-3933.2010.00920.x , archivePrefix =. 1004.3403 , primaryClass =

    work page doi:10.1111/j.1745-3933.2010.00920.x 2010

  31. [31]

    arXiv e-prints , keywords =

    COSMOS-Web: The emergence of the Hubble Sequence. arXiv e-prints , keywords =. doi:10.48550/arXiv.2502.03532 , archivePrefix =. 2502.03532 , primaryClass =

    work page doi:10.48550/arxiv.2502.03532

  32. [32]

    arXiv e-prints , keywords =

    COSMOS2025: The COSMOS-Web galaxy catalog of photometry, morphology, redshifts, and physical parameters from JWST, HST, and ground-based imaging. arXiv e-prints , keywords =. doi:10.48550/arXiv.2506.03243 , archivePrefix =. 2506.03243 , primaryClass =

    work page doi:10.48550/arxiv.2506.03243

  33. [33]

    Mass assembly in quiescent and star-forming galaxies since z=4 from UltraVISTA

    Mass assembly in quiescent and star-forming galaxies since z = 4 from UltraVISTA. AAP , keywords =. doi:10.1051/0004-6361/201321100 , archivePrefix =. 1301.3157 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201321100

  34. [34]

    APJ , keywords =

    The Rapid Buildup of Massive Early-type Galaxies: Supersolar Metallicity, High Velocity Dispersion, and Young Age for an Early-type Galaxy at z = 3.35. APJ , keywords =. doi:10.3847/1538-4357/abc7c4 , archivePrefix =. 2011.04657 , primaryClass =

    work page doi:10.3847/1538-4357/abc7c4 2011

  35. [35]

    Sizes, Colour gradients and Resolved Stellar Mass Distributions for the Massive Cluster Galaxies in XMMUJ2235-2557 at z = 1.39

    Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 at z = 1.39. MNRAS , keywords =. doi:10.1093/mnras/stw502 , archivePrefix =. 1603.00468 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw502

  36. [36]

    Colour gradients in cluster ellipticals at z~1.4: the hidden content of the galaxy central regions

    Colour gradients in cluster ellipticals at z 1.4: the hidden content of the galaxy central regions. MNRAS , keywords =. doi:10.1093/mnras/stx003 , archivePrefix =. 1701.02736 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx003

  37. [37]

    R., Kauffmann, O

    COSMOS2020: A Panchromatic View of the Universe to z 10 from Two Complementary Catalogs. ApJS , keywords =. doi:10.3847/1538-4365/ac3078 , archivePrefix =. 2110.13923 , primaryClass =

    work page doi:10.3847/1538-4365/ac3078

  38. [38]

    , keywords =

    The ages and metallicities of galaxies in the local universe. MNRAS , keywords =. doi:10.1111/j.1365-2966.2005.09321.x , archivePrefix =. astro-ph/0506539 , primaryClass =

    work page doi:10.1111/j.1365-2966.2005.09321.x 2005

  39. [39]

    Predicting Quiescence: The Dependence of Specific Star Formation Rate on Galaxy Size and Central Density at 0.5<z<2.5

    Predicting Quiescence: The Dependence of Specific Star Formation Rate on Galaxy Size and Central Density at 0.5 < z < 2.5. APJ , keywords =. doi:10.3847/1538-4357/aa6258 , archivePrefix =. 1607.03107 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa6258

  40. [40]

    Cluster and field elliptical galaxies at z~1.3. The marginal role of the environment and the relevance of the galaxy central regions

    Cluster and field elliptical galaxies at z 1.3. The marginal role of the environment and the relevance of the galaxy central regions. AAP , keywords =. doi:10.1051/0004-6361/201628866 , archivePrefix =. 1609.06726 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201628866

  41. [41]

    AAP , keywords =

    DAWN JWST Archive: Morphology from profile fitting of over 340 000 galaxies in major JWST fields: Morphology evolution with redshift and galaxy type. AAP , keywords =. doi:10.1051/0004-6361/202555504 , archivePrefix =. 2505.21622 , primaryClass =

    work page doi:10.1051/0004-6361/202555504

  42. [42]

    Celotti and G

    A census of metals and baryons in stars in the local Universe. MNRAS , keywords =. doi:10.1111/j.1365-2966.2007.12632.x , archivePrefix =. 0708.0533 , primaryClass =

    work page doi:10.1111/j.1365-2966.2007.12632.x 2007

  43. [43]

    Evolution of Density Profiles in High-z Galaxies: Compaction and Quenching Inside-Out

    Evolution of density profiles in high-z galaxies: compaction and quenching inside-out. MNRAS , keywords =. doi:10.1093/mnras/stw303 , archivePrefix =. 1509.00017 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw303

  44. [44]

    Wet Disc Contraction to Galactic Blue Nuggets and Quenching to Red Nuggets

    Wet disc contraction to galactic blue nuggets and quenching to red nuggets. MNRAS , keywords =. doi:10.1093/mnras/stt2331 , archivePrefix =. 1310.1074 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt2331

  45. [45]

    Compaction and Quenching of High-z Galaxies in Cosmological Simulations: Blue and Red Nuggets

    Compaction and quenching of high-z galaxies in cosmological simulations: blue and red nuggets. MNRAS , keywords =. doi:10.1093/mnras/stv740 , archivePrefix =. 1412.4783 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv740