Pith. sign in

REVIEW 3 major objections 4 minor 289 references

A cosmic collision in the making: JWST/NIRISS reveals a merging and maturing protocluster core at z~3 around a red quasar

T0 review · 3 major / 4 minor · reviewed 2026-08-14 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read JWST/NIRISS spectroscopy shows the field around the red quasar J1652 is a dense, merging protocluster core at z≈3 with at least 18 member galaxies.

desk verdict A genuinely useful protocluster discovery with a solid characterization of density and passive galaxies, but the merger claim in the title is not established by the paper's own statistics. read the letter →

arxiv 2608.10070 v1 pith:M55QBD2W submitted 2026-08-10 astro-ph.GA

C. Bertemes , D. Wylezalek , G. Noirot , R. Hviding , D. S. N. Rupke , N. L. Zakamska , S. Veilleux , L. Gatto
show 5 more authors
W. Liu A. Vayner Y. Ishikawa Y. Chen S. Sankar
This is my paper · ORCID
classification astro-ph.GA
keywords protoclustercoreJWST/NIRISSslitlessspectroscopyredquasargalaxyoverdensityquiescentgalaxieshalomergerz=3
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper reports the discovery of 'The Step', a dense protocluster at redshift z≈3 found in JWST/NIRISS slitless spectroscopy around the luminous red quasar J1652. It identifies at least 18 member galaxies and argues, from their positions and line-of-sight velocities, that the system contains two substructures arranged in a step-like pattern that may be two dark-matter haloes in the middle of a merger. If that interpretation holds, the structure would be one of the densest known at this epoch, with a halo mass of $13.1 < \log M_{\rm halo}/M_\odot < 13.8$, and a plausible progenitor of a massive, Coma-like cluster at $z=0$. The presence of two quiescent galaxies, a starbursting quasar, and tentative AGN enhancement also makes it a test case for how protocluster environments build and quench massive galaxies.

What carries the argument

The load-bearing object is 'The Step' itself: the step-like distribution of member galaxies in 3D position–velocity space, where the velocity axis doubles as a line-of-sight distance axis. The machinery that produces it is JWST/NIRISS Wide-Field Slitless Spectroscopy: two orthogonal grisms give independent, contamination-checked spectra, and member redshifts are secured by detecting two spectral features ([O ii] and [O iii] emission, or a 4000 Å break with Ca H and K absorption). The paper then converts observed redshifts into velocity offsets from the quasar, splits the sample into a main halo and an infalling subgroup, and compares the resulting kinematics to simulations of single haloes versus halo mergers. That comparison, using the SpiderWeb protocluster as a template, is what carries the claim that the step reflects a merger of two haloes rather than a single virialised system.

What would settle it

Measure secure redshifts with precision better than about 100 km/s for all 18 suspected members (for example with JWST/NIRSpec) and re-examine the velocity distribution; if no step or bimodality remains, or if a single Gaussian fits just as well, the two-halo merger claim fails. A complementary falsifier is a deep X-ray search between the northern and southern groups: a merger should heat an intracluster medium, while its absence would argue against the system being a single collapse-bound structure.

Watch

Extended reading notes

Core claim

The central discovery is that the quasar J1652 sits in an exceptionally dense, still-assembling protocluster core. Using two orthogonal grisms on NIRISS, the paper spectroscopically confirms 18 member galaxies within $\pm 2000$ km/s of the quasar, including 12 new line emitters, two passive galaxies identified by strong 4000 Å breaks, and two new AGN candidates. In the 3D position–velocity diagram the members separate into a northern, strongly blueshifted group and a southern, more clustered group, producing a step-like pattern that the authors interpret as two merging haloes rather than a single relaxed structure. They derive a galaxy overdensity of a factor >100 in a $320\times230$ kpc$^2$ core and >15 over the 1 Mpc$^2$ field, and a halo mass range between $\log M_{\rm halo}/M_\odot = 13.1$ and $13.8$, which maps onto the expected progenitor mass range for today's Coma-like clusters. The mix of active star formation, quiescent galaxies, and AGN candidates places the system in an emerging class of 'maturing' protoclusters at $z\approx2$–$4$, a regime proposed as the transition between early star-forming overdensities and the passive galaxy cores of local clusters.

Load-bearing premise

The load-bearing premise is that the step-like split in the position–velocity diagram reflects two real merging haloes rather than noise from the 380 km/s redshift uncertainty; on only 18 members the paper's own Gaussian tests cannot distinguish the two.

Editorial extensions

If this is right

  • If the merger interpretation is right, the Step is a direct, caught-in-the-act example of hierarchical assembly of a massive cluster core at $z\approx3$.
  • The two quiescent galaxies imply that quiescence can set in even in overdense, actively star-forming environments, consistent with an environmentally accelerated quenching pathway.
  • With halo mass $13.1<\log M_{\rm halo}/M_\odot<13.8$ and overdensity $\delta>15$, the structure is a candidate progenitor of a Coma-like cluster at $z=0$, so its eventual descendant could be identified among today's massive local clusters.
  • A tentatively elevated AGN fraction (10–20%) suggests that the dense, merging core is also a site of enhanced black-hole growth, linking halo assembly to AGN feedback at the epoch just before cluster cores turn passive.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The step's statistical footing is thinner than its visual impression: the paper's own Kolmogorov–Smirnov and Shapiro–Wilk tests do not reject a Gaussian velocity distribution, so a reader should treat the two-halo merger as a motivated hypothesis rather than a measured bimodality.
  • A direct test would be to obtain per-member redshifts with precision well below 100 km/s across the full 1 Mpc$^2$ field; if the step persists, the merger scenario gains real support, and if it washes out the system may be a single, elongated, non-virialised halo.
  • Future X-ray observations could look for diffuse hot intracluster medium between the two groups, as has been claimed for the SpiderWeb protocluster core; its presence would confirm that the merger is actually heating a forming ICM.
  • The paper implicitly predicts that wide-area, deep spectroscopy around J1652 should find more low-mass members on the southern side and possibly an extended filament connecting the two groups; a missing filament would weaken the single-descendant-cluster outcome.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. Bertemes et al. present JWST/NIRISS wide-field slitless spectroscopy of the field around the red quasar SDSS J1652 at z=2.9489. They report 18 spectroscopically confirmed protocluster members, including two quiescent galaxies with D4000 breaks, two AGN candidates, and two broad-[OIII] sources. The authors measure a galaxy overdensity of >100 in a 320x230 kpc^2 core and >15 in the ~1 Mpc^2 field, and estimate a halo mass of log M_halo/M_sun = 13.1-13.8, suggesting the system could evolve into a Coma-like cluster. They note a step-like structure in the 3D position-velocity distribution and propose that the system is undergoing a merger of two halos. The paper also compares the star-formation activity and passive fraction with field galaxies and other protoclusters, concluding that the system is in a transitional, maturing phase at z~3.

Significance. The protocluster discovery itself is significant: 18 members with two spectral features each in a compact region around a luminous quasar is a valuable addition to the small sample of spectroscopically confirmed, high-density structures at z>2. The presence of two massive quiescent galaxies, together with tentative AGN candidates, supports the emerging picture that z~3 is a maturation epoch for protoclusters. However, the merger interpretation, which drives the title and part of the narrative, is not validated by the presented statistics; the KS/Shapiro-Wilk tests fail to reject a single Gaussian, and the substructure is identified by eye. The paper would be more convincing if the merger claims were toned down or supported by a quantitative test. The strengths of the paper are the transparent discussion of systematic uncertainties, the two-feature spectroscopic confirmation, and the detailed comparison to literature systems.

major comments (3)
  1. [Section 3.2 and Section 3.5, Fig. 5] The claim that the protocluster exhibits two substructures in 3D position-velocity space and may be undergoing a merger of two haloes is not supported by any quantitative test. The KS and Shapiro-Wilk tests reported in Section 3.2 do not reject a Gaussian velocity distribution, and Section 3.5 explicitly concedes that the number statistics are too low to confirm or reject a double-peaked distribution. The visual identification of the step in Fig. 5 and the by-eye assignment of IDs 1-6 and 15 to a northern structure are not robust to the adopted redshift uncertainty of dz=0.005 (380 km/s), which is comparable to the 700-850 km/s velocity span within the core and a non-negligible fraction of the ~1200 km/s separation between the nominal groups. Therefore the merging and maturing protocluster in the title and abstract overstates the evidence. Please either remove the merger language from the title/abstract and Section 4, or add a quantitative test (e.g., a two-component Gaussian mixture with a likelihood-ratio or bootstrap null against a single skewed distribution) and present the merger as one of several possible interpretations, including the SSA22-like chance alignment discussed in Section 3.5.
  2. [Section 3.3] The galaxy overdensity factors (>15 for the full field, >100 for the core) depend on the assumed field mass-function cutoff at log M*/M_sun = 9.14, taken as the mass of the least massive member. However, the stellar masses are derived from a constant mass-to-light ratio with a plausible spread of ±0.5 dex (Section 3.3), and the sample is emission-line selected, so the completeness as a function of stellar mass is not established. A shift in the adopted mass cutoff by ±0.5 dex would change the field density and hence δ by a factor that is not quantified. Please provide an uncertainty estimate on δ propagating the stellar-mass uncertainty and sample incompleteness, or explicitly report δ as a lower limit with these caveats, to support the claim that this is one of the densest structures known at this redshift.
  3. [Section 3.4] The halo mass range 13.1 < log M_halo/M_sun < 13.8 underpins the conclusion that the structure could evolve into a Coma-like cluster at z=0. This range is drawn from two external calibrations (Evrard et al. 2008 velocity-dispersion scaling and Shuntov et al. 2022 SMHM relation), both of which carry systematic uncertainties. The dynamical mass is an upper limit because the system is not virialised, and the SMHM-derived mass is explicitly a lower limit due to field-of-view limitations. More importantly, if the system is a chance superposition of two groups rather than a single collapsing halo (the SSA22 alternative discussed in Section 3.5), the combined halo mass is not the mass of a single descendant at z=0. Please either (a) add a sensitivity analysis that shows how the halo mass range changes under the merger vs. single-halo hypotheses, or (b) soften the conclusion about the system being a likely Coma progenitor to reflect this uncertainty.
minor comments (4)
  1. [Abstract and Section 3.2] The abstract states that seven galaxies lie within 70 projected kpc from the quasar, while Section 3.2 reports six galaxies (IDs 7, 8, 9, 10, 11, 12) within that radius; please clarify whether the quasar is counted in these numbers to avoid an apparent inconsistency.
  2. [Section 1] The sentence 'we use a we use a ΛCDM cosmology' contains a duplicated phrase; please correct the typo.
  3. [Section 2.3] The phrase 'to this end' at the start of the second paragraph should be capitalized as 'To this end'.
  4. [Fig. 5 caption] The dashed line indicating the step in the 3D view is a guide to the eye, but the caption does not state that it is not a fitted model; please add a sentence noting that the step is a subjective visual annotation rather than a quantitative decomposition.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: member selection, overdensity, and halo mass rest on external calibrations and independent NIRSpec data; the merger claim is weakly supported but not circular.

full rationale

The paper's claimed derivations are self-contained against external, non-fitted inputs. Protocluster members are selected by requiring two spectral features in both orthogonal grisms (Section 2.3), not by fitting the target overdensity or halo mass. The galaxy overdensity uses the Weaver et al. (2023) z=3 stellar mass function as the field reference; the halo mass uses the Evrard et al. (2008) velocity-dispersion scaling and the Shuntov et al. (2022) stellar-mass-halo-mass relation; SFRs use Kennicutt & Evans (2012) and the Popesso et al. (2023) main sequence; the AGN and passive fractions are compared to externally measured field values (Bongiorno et al. 2016; Arango-Toro et al. 2025). None of these calibrations is fit to the paper's own results, so the overdensity, halo mass, and fractions are not forced by construction. The self-citations (Wylezalek et al. 2022; Chen et al. 2026; Bertemes et al. 2025) provide NIRSpec companion redshifts, the quasar stellar mass, and black-hole mass from independent data; they are supporting evidence, and the NIRISS sample adds 12 new sources independent of them. The title's merging scenario is an interpretation of the same observed velocity distribution, but the paper explicitly concedes the statistical weakness: Section 3.2 reports that Kolmogorov-Smirnov and Shapiro-Wilk tests do not reject a Gaussian null, and Section 3.5 states that 'the number statistics are too low to confirm or reject a double-peaked distribution in the velocity histogram.' This is a limitation on the merger claim, not a circular reduction of a predicted quantity to an input. No equation in the paper equates a derived result to a fitted parameter or to a self-cited theorem, so no circular step is present.

Assumptions & free parameters 4 free parameters · 7 assumptions · 0 invented entities

The central claims depend on several hand-picked assumptions (dust extinction, mass-to-light ratio, attenuation ratio, redshift error) and on external calibrations from the literature. None are fitted to the target data, but the systematic uncertainties they introduce are comparable to the reported effects, so the quantitative conclusions (SFR offset, halo mass, AGN fraction) should be treated as order-of-magnitude estimates.

free parameters (4)
  • Fiducial dust extinction A_V = 0.7 mag
    Assumed for all member galaxies at z=3; affects SFR and stellar mass estimates. The authors note it could vary from 0 to 1.5 mag, changing stellar masses by ±0.3 dex.
  • Mass-to-light ratio log(M*/L_B) = -0.3 (solar units)
    Assumed for a 1 Gyr-old stellar population (Maraston 2005); plausible range 0.16 to 1.6, giving ±0.5 dex uncertainty in stellar masses, which feed the overdensity limit, passive fraction, and SMHM-based halo mass.
  • Stellar-to-nebular attenuation ratio = 0.67
    Taken from Shen et al. (2025); used to correct H-beta based SFRs for dust attenuation.
  • Adopted redshift uncertainty = 0.005 (uniform)
    Chosen conservatively to account for calibration systematics; corresponds to 380 km/s at z=3 and directly affects the significance of the velocity substructure and the merger interpretation.
assumptions (7)
  • standard math Flat Lambda-CDM cosmology with Omega_m=0.3, Omega_Lambda=0.7, H0=70 km/s/Mpc
    Stated in Section 1; used for distance and volume calculations.
  • standard math Case B recombination H-alpha/H-beta = 2.85 for star-forming galaxies
    Used in Section 3.3 to convert observed H-beta flux to H-alpha for SFR estimates.
  • domain assumption Kennicutt & Evans (2012) H-alpha to SFR calibration
    Adopted in Section 3.3 to derive SFRs; the authors note metallicity could lower SFRs by a factor ~1.8.
  • domain assumption Velocity dispersion to halo mass scaling from Evrard et al. (2008) and Sifon et al. (2013)
    Used in Section 3.4 to estimate dynamical halo mass; the authors note non-virialization can overestimate the mass by ~0.5 dex.
  • domain assumption Stellar mass-halo mass relation at z=3 from Shuntov et al. (2022)
    Used in Section 3.4 to obtain a halo mass of log M_halo/M_sun = 13.1-13.2 from the summed stellar mass of members.
  • domain assumption Observed redshift differences can be interpreted as either spatial separation or peculiar velocity
    Stated in Section 2.3; underpins the 3D structure in Fig 5 and the volume used for the overdensity calculation.
  • domain assumption Weaver et al. (2023) stellar mass function at z=3 as the field baseline
    Used in Section 3.3 to compute the field galaxy density; effects of incompleteness and mass errors propagate into the overdensity factor.

how reviews work

0 comments
Cite this review

Pith. "Pith review of A cosmic collision in the making: JWST/NIRISS reveals a merging and maturing protocluster core at z~3 around a red quasar." pith.science (2026). https://pith.science/paper/M55QBD2W

@misc{pith2026260810070,
  author       = {Pith},
  title        = {Pith review of: A cosmic collision in the making: JWST/NIRISS reveals a merging and maturing protocluster core at z~3 around a red quasar},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/M55QBD2W}},
  note         = {Machine review of arXiv:2608.10070}
}
abstract

We report the discovery of ``The Step'', a dense protocluster at z=3 revealed by JWST/NIRISS Wide-Field Slitless Spectroscopy (WFSS) of the field around the luminous quasar and starburst SDSSJ165202.64+172852.3. The protocluster contains at least 18 member galaxies and exhibits two substructures in the 3D position-velocity space - notably a distinctive step-like distribution, from which the nickname derives. We propose that the Step may be undergoing a merger of two haloes, which could also explain the large velocity span (700-850km/s) between galaxies along the densest line of sight. This sightline contains seven galaxies within 70 projected kpc from the quasar, consistent with a remarkably dense protocluster core. We derive a galaxy overdensity of a factor >100 in the core and >15 within 1 Mpc$^2$, making it one of the densest structures known at this redshift, and a very massive halo of $13.1 < log M_{\rm halo}/ M_\odot < 13.8$, which suggests the structure could potentially evolve into a massive, Coma-like cluster at z=0. Compared to the field, the star-forming galaxies in the Step show slightly elevated levels of star formation. Yet, we find two quiescent galaxies with strong D4000 breaks and no evidence for ongoing star formation. Compared to other z=3 protoclusters, the Step exhibits similar or slightly suppressed star-forming activity. We also identify two new AGN candidates and find tentative evidence for an enhanced AGN fraction (10-20%) compared to the field. The protocluster constitutes one of the emerging handful of maturing structures at 2 < z < 4 that host both star-forming and quenched galaxies. This redshift regime may thus be a key transitional epoch for cluster studies, where overdensities transition from being the most active sites of star formation in the early Universe towards shaping the massive passive ellipticals seen in the cores of today's clusters.

Figures

Figures reproduced from arXiv: 2608.10070 by the authors.

Figure 1
Figure 1. Spectra and recovered redshift probability distribution of a representative star-forming galaxy and the two passive galaxies, [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. 2D NIRISS spectra of the representative star-forming pro [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Overview of the protocluster field targeted by JWST/NIRISS. The spectroscopically confirmed cluster members (diamond symbols) are colour-coded by the (projected) velocity offset from the central source as well as redshift. The 3′′x3′′ field of view of the JWST/NIRSpec observations - which contains the quasar and 3 galaxies within a projected distance of < 20 kpc - is overplotted in red in the centre. (Sommariva et a… view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: Distribution of the line-of-sight velocity o [PITH_FULL_IMAGE:figures/full_fig_p008_4.png]
Figure 5
Figure 5. Figure 5: 3D visualisation of the protocluster’s structure. The quasar is marked by a star symbol, and the IDs from Table 1 are annotated. [PITH_FULL_IMAGE:figures/full_fig_p009_5.png]
Figure 6
Figure 6. Figure 6: SFR-M⋆ plane with the z = 3 star-forming Main Se￾quence (Popesso et al. 2023). The grey open diamond shows the median SFR and M⋆ of our sample (excluding the passive galaxies and quasar). We use our best estimates of the individual SFRs and stellar masses to tentativel…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

289 extracted references · 3 canonical work pages

  1. [1]

    doi:10.1093/mnras/stab3089 , eprint =

    , keywords =. doi:10.1093/mnras/stab3089 , eprint =

    doi:10.1093/mnras/stab3089

  2. [2]

    , keywords =

    An excess of dusty starbursts related to the Spiderweb galaxy. , keywords =. doi:10.1051/0004-6361/201423771 , archivePrefix =. 1410.3730 , primaryClass =

    arXiv

  3. [4]

    A Search for clusters at high redshift. I. Candidate Lyalpha emitters near 1138-262 at z=2.2. , keywords =. doi:10.48550/arXiv.astro-ph/0005058 , archivePrefix =. astro-ph/0005058 , primaryClass =

    arXiv doi:10.48550/arxiv.astro-ph/0005058

  4. [5]

    , keywords =

    The first appearance of the red sequence of galaxies in proto-clusters at 2 < -0.5ex z < -0.5ex 3. , keywords =. doi:10.1111/j.1365-2966.2007.11739.x , archivePrefix =. astro-ph/0703382 , primaryClass =

    arXiv 2007

  5. [6]

    , keywords =

    The Filamentary Large-Scale Structure around the z=2.16 Radio Galaxy PKS 1138-262. , keywords =. doi:10.1086/431956 , archivePrefix =. astro-ph/0505354 , primaryClass =

    arXiv

  6. [7]

    A search for clusters at high redshift. IV. Spectroscopy of H emitters in a proto-cluster at z = 2.16. , keywords =. doi:10.1051/0004-6361:20041819 , archivePrefix =. astro-ph/0410203 , primaryClass =

    arXiv

  7. [8]

    , keywords =

    The Spiderweb Galaxy: A Forming Massive Cluster Galaxy at z -0.5ex 2. , keywords =. doi:10.1086/508534 , archivePrefix =. astro-ph/0610909 , primaryClass =

    arXiv

  8. [9]

    , keywords =

    The Massive Hosts of Radio Galaxies across Cosmic Time. , keywords =. doi:10.1086/517887 , archivePrefix =. astro-ph/0703224 , primaryClass =

    arXiv

Show all 289 references
  1. [10]

    The 700 ks Chandra Spiderweb Field. I. Evidence for widespread nuclear activity in the protocluster. , keywords =. doi:10.1051/0004-6361/202142333 , archivePrefix =. 2203.02208 , primaryClass =

    arXiv

  2. [11]

    arXiv e-prints , keywords =

    DeepDive: Simultaneous Formation of Massive Quiescent Galaxies in High-Redshift Galaxy Proto-clusters. arXiv e-prints , keywords =. doi:10.48550/arXiv.2604.21007 , archivePrefix =. 2604.21007 , primaryClass =

    doi arXiv

  3. [12]

    A search for clusters at high redshift. II. A proto cluster around a radio galaxy at z=2.16. , keywords =. doi:10.48550/arXiv.astro-ph/0008143 , archivePrefix =. astro-ph/0008143 , primaryClass =

    doi arXiv

  4. [13]

    , keywords =

    A Large Structure of Galaxies at Redshift Z approximately 3 and Its Cosmological Implications. , keywords =. doi:10.1086/305073 , archivePrefix =. astro-ph/9708125 , primaryClass =

    arXiv

  5. [14]

    , keywords =

    Clusters of Galaxies in the First Half of the Universe from the IRAC Shallow Survey. , keywords =. doi:10.1086/590105 , archivePrefix =. 0804.4798 , primaryClass =

    arXiv

  6. [15]

    , keywords =

    Low ionization active galactic nuclei : X-ray or shock heated ?. , keywords =. doi:10.1086/184051 , adsurl =

    doi

  7. [16]

    , keywords =

    Improved Empirical Backgrounds for JWST NIRISS Image/Wide-field Slitless Spectroscopy Data Reduction. , keywords =. doi:10.3847/1538-3881/ad82ee , archivePrefix =. 2410.00103 , primaryClass =

    arXiv

  8. [17]

    The incidence of AGN as a function of star formation rate

    X-rays across the galaxy population - III. The incidence of AGN as a function of star formation rate. , keywords =. doi:10.1093/mnras/stz125 , archivePrefix =. 1810.04683 , primaryClass =

    arXiv

  9. [18]

    , keywords =

    Ancient Light from Young Cosmic Cities: Physical and Observational Signatures of Galaxy Proto-clusters. , keywords =. doi:10.1088/0004-637X/779/2/127 , archivePrefix =. 1310.2938 , primaryClass =

    arXiv

  10. [20]

    , keywords =

    A lensed protocluster candidate at z = 7.66 identified in JWST observations of the galaxy cluster SMACS0723 - 7327. , keywords =. doi:10.1051/0004-6361/202244719 , archivePrefix =. 2208.04930 , primaryClass =

    arXiv

  11. [21]

    doi:10.5281/zenodo.7628094 , url =

    Matharu, Jasleen and Brammer, Gabriel , title =. doi:10.5281/zenodo.7628094 , url =

    doi

  12. [23]

    2016 , publisher =

    Kyle Barbary , title =. 2016 , publisher =. doi:10.21105/joss.00058 , url =

    2016 doi

  13. [24]

    The Propagation of Uncertainties in Stellar Population Synthesis Modeling. I. The Relevance of Uncertain Aspects of Stellar Evolution and the Initial Mass Function to the Derived Physical Properties of Galaxies. , keywords =. doi:10.1088/0004-637X/699/1/486 , archivePrefix =. ...

    arXiv

  14. [25]

    The Propagation of Uncertainties in Stellar Population Synthesis Modeling. III. Model Calibration, Comparison, and Evaluation. , keywords =. doi:10.1088/0004-637X/712/2/833 , archivePrefix =. 0911.3151 , primaryClass =

    arXiv

  15. [26]

    , keywords =

    Spectroscopic Confirmation of a Protocluster at z 3.786. , keywords =. doi:10.3847/0004-637X/823/1/11 , archivePrefix =. 1604.08627 , primaryClass =

    arXiv

  16. [27]

    , keywords =

    Spectroscopic observations of PHz G237.01+42.50: A galaxy protocluster at z = 2.16 in the Cosmos field. , keywords =. doi:10.1051/0004-6361/202140612 , archivePrefix =. 2109.04396 , primaryClass =

    arXiv

  17. [28]

    , keywords =

    VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster at z -0.5ex 3.3. , keywords =. doi:10.1051/0004-6361/201423828 , archivePrefix =. 1403.4230 , primaryClass =

    arXiv

  18. [29]

    , keywords =

    Discovery of a rich proto-cluster at z = 2.9 and associated diffuse cold gas in the VIMOS Ultra-Deep Survey (VUDS). , keywords =. doi:10.1051/0004-6361/201423811 , archivePrefix =. 1403.3691 , primaryClass =

    arXiv

  19. [30]

    , keywords =

    COSMOS2020: Identification of High-z Protocluster Candidates in COSMOS. , keywords =. doi:10.3847/1538-4357/ac9d96 , archivePrefix =. 2210.17334 , primaryClass =

    arXiv

  20. [31]

    , keywords =

    COSMOS2020: Cosmic evolution of the stellar-to-halo mass relation for central and satellite galaxies up to z 5. , keywords =. doi:10.1051/0004-6361/202243136 , archivePrefix =. 2203.10895 , primaryClass =

    arXiv

  21. [32]

    , keywords =

    GA-NIFS: The core of an extremely massive protocluster at the epoch of reionisation probed with JWST/NIRSpec. , keywords =. doi:10.1051/0004-6361/202348824 , archivePrefix =. 2312.00899 , primaryClass =

    arXiv

  22. [33]

    , keywords =

    The AGN fraction in high-redshift protocluster candidates selected by Planck and Herschel. , keywords =. doi:10.1093/mnras/stad3404 , archivePrefix =. 2311.01658 , primaryClass =

    arXiv

  23. [34]

    , keywords =

    Virial Scaling of Massive Dark Matter Halos: Why Clusters Prefer a High Normalization Cosmology. , keywords =. doi:10.1086/521616 , archivePrefix =. astro-ph/0702241 , primaryClass =

    arXiv

  24. [35]

    , keywords =

    H -derived Star Formation Rates for Three z -0.5ex =0.75 EDisCS Galaxy Clusters. , keywords =. doi:10.1086/431642 , archivePrefix =. astro-ph/0504578 , primaryClass =

    arXiv

  25. [36]

    , keywords =

    The Atacama Cosmology Telescope: Dynamical Masses and Scaling Relations for a Sample of Massive Sunyaev-Zel'dovich Effect Selected Galaxy Clusters. , keywords =. doi:10.1088/0004-637X/772/1/25 , archivePrefix =. 1201.0991 , primaryClass =

    arXiv

  26. [37]

    The assembly and star formation cessation of galaxies at 0.2< z 7.5

    COSMOS2020: The galaxy stellar mass function. The assembly and star formation cessation of galaxies at 0.2< z 7.5. , keywords =. doi:10.1051/0004-6361/202245581 , archivePrefix =. 2212.02512 , primaryClass =

    arXiv

  27. [38]

    , keywords =

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

    arXiv

  28. [39]

    Is AGN feedback responsible for the mass-quenching of galaxies?

    AGN host galaxy mass function in COSMOS. Is AGN feedback responsible for the mass-quenching of galaxies?. , keywords =. doi:10.1051/0004-6361/201527436 , archivePrefix =. 1601.02091 , primaryClass =

    arXiv

  29. [40]

    , keywords =

    Evidence of Extreme Ionization Conditions and Low Metallicity in GHZ2/GLASS-Z12 from a Combined Analysis of NIRSpec and MIRI Observations. , keywords =. doi:10.3847/1538-4357/ad7602 , archivePrefix =. 2403.12683 , primaryClass =

    arXiv

  30. [41]

    , keywords =

    CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3. , keywords =. doi:10.3847/1538-4357/ac8058 , archivePrefix =. 2205.05090 , primaryClass =

    arXiv

  31. [42]

    , keywords =

    Theoretical Evolution of Optical Strong Lines across Cosmic Time. , keywords =. doi:10.1088/0004-637X/774/2/100 , archivePrefix =. 1307.0508 , primaryClass =

    arXiv

  32. [43]

    Nature Astronomy , keywords =

    Impact of supermassive black hole growth on star formation. Nature Astronomy , keywords =. doi:10.1038/s41550-017-0165 , archivePrefix =. 1703.06889 , primaryClass =

    arXiv

  33. [44]

    , keywords =

    The main sequence of star-forming galaxies across cosmic times. , keywords =. doi:10.1093/mnras/stac3214 , archivePrefix =. 2203.10487 , primaryClass =

    arXiv

  34. [45]

    q3dfit: PSF decomposition and spectral analysis for JWST-IFU spectroscopy

  35. [46]

    arXiv , author =:1411.1431 , journal =

    doi:10.1088/2041-8205/801/1/L12 , eid =. arXiv , author =:1411.1431 , journal =

    arXiv

  36. [47]

    , keywords =

    COSMOS2020: Discovery of a Protocluster of Massive Quiescent Galaxies at z = 2.77. , keywords =. doi:10.3847/2041-8213/acb49b , archivePrefix =. 2301.08845 , primaryClass =

    arXiv

  37. [48]

    ApJ , keywords =

    The Ubiquity of Coeval Starbursts in Massive Galaxy Cluster Progenitors. ApJ , keywords =. doi:10.3847/0004-637X/824/1/36 , archivePrefix =. 1603.04437 , primaryClass =

    arXiv

  38. [49]

    , keywords =

    Molecular gas properties of Planck-selected protocluster candidates at z ≃ 1.3-3. , keywords =. doi:10.1051/0004-6361/202142255 , archivePrefix =. 2203.13183 , primaryClass =

    arXiv

  39. [50]

    , keywords =

    Planck Far-infrared Detection of Hyper Suprime-Cam Protoclusters at z 4: Hidden AGN and Star Formation Activity. , keywords =. doi:10.3847/1538-4357/ab5a80 , archivePrefix =. 1911.09368 , primaryClass =

    1911 arXiv

  40. [51]

    , keywords =

    ALMA observations of a z 3.1 protocluster: star formation from active galactic nuclei and Lyman-alpha blobs in an overdense environment. , keywords =. doi:10.1093/mnras/stw1509 , archivePrefix =. 1601.00682 , primaryClass =

    arXiv

  41. [52]

    , keywords =

    Galaxy morphology in rich clusters: implications for the formation and evolution of galaxies. , keywords =. doi:10.1086/157753 , adsurl =

    doi

  42. [53]

    arXiv , author =:1604.00016 , journal =

    doi:10.3847/0004-637X/832/1/7 , eid =. arXiv , author =:1604.00016 , journal =

    arXiv

  43. [54]

    arXiv , author =:2401.14567 , journal =

    doi:10.48550/arXiv.2401.14567 , eid =. arXiv , author =:2401.14567 , journal =

    doi

  44. [55]

    Monthly Notices of the Royal Astronomical Society , keywords =

    Accurso, G and Saintonge, A and Catinella, B and Cortese, L and Dav. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stx1556 , eprint =

    doi

  45. [56]

    arXiv , author =:2108.07812 , journal =

    doi:10.3847/1538-4357/ac1e8d , eid =. arXiv , author =:2108.07812 , journal =

    arXiv

  46. [57]

    , keywords =

    COSMOS-Web: A history of galaxy migrations over the stellar mass star formation rate plane. , keywords =. doi:10.1051/0004-6361/202452519 , adsurl =

    doi

  47. [58]

    doi:10.1093/pasj/psab122 , eprint =

    , keywords =. doi:10.1093/pasj/psab122 , eprint =

    doi

  48. [59]

    arXiv , author =:2208.12490 , journal =

    doi:10.1051/0004-6361/202244162 , eid =. arXiv , author =:2208.12490 , journal =

    arXiv

  49. [60]

    and Wylezalek, D

    Albán, M. and Wylezalek, D. and et al. , journal =. , year =

  50. [61]

    doi:10.3390/universe8110554 , eprint =

    Universe , keywords =. doi:10.3390/universe8110554 , eprint =

    doi

  51. [62]

    , keywords =

    LoCuSS: The Steady Decline and Slow Quenching of Star Formation in Cluster Galaxies over the Last Four Billion Years. , keywords =. doi:10.1088/0004-637X/775/2/126 , archivePrefix =. 1307.1135 , primaryClass =

    arXiv

  52. [63]

    , keywords =

    Star Formation and AGN Activity in Galaxy Clusters from z=1-2: a Multi-Wavelength Analysis Featuring Herschel/PACS. , keywords =. doi:10.3847/0004-637X/825/1/72 , archivePrefix =. 1604.03564 , primaryClass =

    arXiv

  53. [64]

    , keywords =

    Star formation in the cluster CLG0218.3-0510 at z = 1.62 and its large-scale environment: the infrared perspective. , keywords =. doi:10.1093/mnras/stt2376 , archivePrefix =. 1312.1694 , primaryClass =

    arXiv

  54. [65]

    , keywords =

    The reversal of the SF-density relation in a massive, X-ray-selected galaxy cluster at z = 1.58: results from Herschel. , keywords =. doi:10.1093/mnrasl/slu180 , archivePrefix =. 1412.5188 , primaryClass =

    arXiv

  55. [66]

    , keywords =

    The role of massive halos in the star formation history of the Universe. , keywords =. doi:10.1051/0004-6361/201424715 , archivePrefix =. 1407.8231 , primaryClass =

    arXiv

  56. [67]

    , keywords =

    The evolution of galaxy star formation activity in massive haloes. , keywords =. doi:10.1051/0004-6361/201424711 , archivePrefix =. 1407.8214 , primaryClass =

    arXiv

  57. [68]

    , keywords =

    Dusty Starbursts and the Formation of Elliptical Galaxies: A SCUBA-2 Survey of a z = 1.46 Cluster. , keywords =. doi:10.1088/0004-637X/806/2/257 , archivePrefix =. 1504.06630 , primaryClass =

    arXiv

  58. [69]

    , keywords =

    Deciphering the Activity and Quiescence of High-redshift Cluster Environments: ALMA Observations of Cl J1449+0856 at z = 2. , keywords =. doi:10.3847/1538-4357/aacd10 , archivePrefix =. 1806.06856 , primaryClass =

    arXiv

  59. [70]

    , keywords =

    Revealing dust-obscured star formation in CLJ1449+0856, a cluster at z = 2. , keywords =. doi:10.1093/mnras/stz1090 , archivePrefix =. 1904.07246 , primaryClass =

    1904 arXiv

  60. [71]

    , keywords =

    Two sub-millimetre bright protoclusters bounding the epoch of peak star-formation activity. , keywords =. doi:10.1093/mnras/stz1742 , archivePrefix =. 1809.06882 , primaryClass =

    arXiv

  61. [72]

    , keywords =

    The Evolution of the Ultraluminous Infrared Galaxy Population from Redshift 0 to 1.5. , keywords =. doi:10.1086/383198 , archivePrefix =. astro-ph/0402235 , primaryClass =

    arXiv

  62. [73]

    , keywords =

    A Panoramic Mid-Infrared Survey of Two Distant Clusters. , keywords =. doi:10.1086/506469 , archivePrefix =. astro-ph/0606110 , primaryClass =

    arXiv

  63. [74]

    Characterizing massive forming galaxies in the Spiderweb protocluster at z = 2.2

    MAHALO Deep Cluster Survey II. Characterizing massive forming galaxies in the Spiderweb protocluster at z = 2.2. , keywords =. doi:10.1093/mnras/sty2618 , archivePrefix =. 1809.08755 , primaryClass =

    arXiv

  64. [75]

    , keywords =

    Galaxy populations of protoclusters in cosmological hydrodynamical simulations. , keywords =. doi:10.1051/0004-6361/202453507 , archivePrefix =. 2503.01674 , primaryClass =

    arXiv

  65. [76]

    , keywords =

    A Hard Ionizing Spectrum in z = 3-4 Ly Emitters with Intense [O III] Emission: Analogs of Galaxies in the Reionization Era?. , keywords =. doi:10.3847/2041-8205/831/1/L9 , archivePrefix =. 1608.08222 , primaryClass =

    arXiv

  66. [77]

    arXiv e-prints , keywords =

    The birth of the intracluster medium: the evolution of multiphase gas and Lyman- α haloes in a simulated z 3 protocluster. arXiv e-prints , keywords =. doi:10.48550/arXiv.2603.16991 , archivePrefix =. 2603.16991 , primaryClass =

    doi arXiv

  67. [78]

    The 700 ks Chandra Spiderweb Field. II. Evidence for inverse-Compton and thermal diffuse emission in the Spiderweb galaxy. , keywords =. doi:10.1051/0004-6361/202244337 , archivePrefix =. 2209.15467 , primaryClass =

    arXiv

  68. [79]

    , keywords =

    Properties of Ly emitters around the radio galaxy MRC 0316 257 ^ ,. , keywords =. doi:10.1051/0004-6361:20042038 , archivePrefix =. astro-ph/0501259 , primaryClass =

    arXiv

  69. [81]

    , keywords =

    The progeny of a cosmic titan: a massive multi-component proto-supercluster in formation at z = 2.45 in VUDS. , keywords =. doi:10.1051/0004-6361/201833655 , archivePrefix =. 1806.06073 , primaryClass =

    arXiv

  70. [82]

    , keywords =

    Galaxy evolution in protoclusters. , keywords =. doi:10.1093/mnras/stx2454 , archivePrefix =. 1709.07009 , primaryClass =

    arXiv

  71. [83]

    , keywords =

    A massive core for a cluster of galaxies at a redshift of 4.3. , keywords =. doi:10.1038/s41586-018-0025-2 , archivePrefix =. 1804.09231 , primaryClass =

    arXiv

  72. [84]

    Spitzer observations of Abell 1763. III. The infrared luminosity function in different supercluster environments. , keywords =. doi:10.1051/0004-6361/201016174 , archivePrefix =. 1106.1657 , primaryClass =

    arXiv

  73. [86]

    doi:10.1093/mnras/sty1685 , eprint =

    , keywords =. doi:10.1093/mnras/sty1685 , eprint =

    doi

  74. [87]

    , keywords =

    The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: The Spitzer Catalog. , keywords =. doi:10.3847/1538-4357/aa7b89 , archivePrefix =. 1611.00746 , primaryClass =

    arXiv

  75. [88]

    arXiv , author =:2202.11651 , journal =

    doi:10.3847/1538-4357/ac58fb , eid =. arXiv , author =:2202.11651 , journal =

    arXiv

  76. [89]

    arXiv , author =:2303.13469 , journal =

    doi:10.1051/0004-6361/202346489 , eid =. arXiv , author =:2303.13469 , journal =

    arXiv

  77. [90]

    doi:10.1093/mnras/stab780 , eprint =

    , keywords =. doi:10.1093/mnras/stab780 , eprint =

    doi

  78. [91]

    Ground-based and Airborne Instrumentation for Astronomy III , doi =

  79. [92]

    doi:10.1093/mnras/stab3672 , eprint =

    , keywords =. doi:10.1093/mnras/stab3672 , eprint =

    doi

  80. [93]

    arXiv , author =:2210.03755 , journal =

    arXiv

  81. [94]

    doi:10.1093/mnras/stw1984 , eprint =

    , keywords =. doi:10.1093/mnras/stw1984 , eprint =

    doi

  82. [95]

    arXiv , author =:2305.14418 , journal =

    doi:10.3847/1538-4357/ad167e , eid =. arXiv , author =:2305.14418 , journal =

    arXiv

  83. [97]

    doi:10.1086/176166 , journal =

    doi

  84. [98]

    The Astrophysical Journal , pages =

    Behroozi, Peter S and Wechsler, Risa H and Conroy, Charlie , doi =. The Astrophysical Journal , pages =

  85. [99]

    doi:10.1093/mnras/stx789 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stx789 , eprint =

    doi

  86. [100]

    arXiv , author =:1901.00866 , journal =

    doi:10.3847/1538-3881/ab3e4e , eid =. arXiv , author =:1901.00866 , journal =

    1901 arXiv

  87. [101]

    arXiv , author =:2111.14876 , journal =

    arXiv

  88. [102]

    arXiv , author =:1608.00608 , journal =

    doi:10.3847/1538-4357/834/1/18 , eid =. arXiv , author =:1608.00608 , journal =

    arXiv

  89. [103]

    , journal =

    Bertemes, Caroline and Wylezalek, Dominika and et al. , journal =. , volume =

  90. [104]

    and Wuyts, S

    Bertemes, C. and Wuyts, S. and et al. , journal =. , year =

  91. [105]

    and Wuyts, S

    Bertemes, C. and Wuyts, S. , journal =. , year =

  92. [106]

    , keywords =

    A Candidate Brightest Protocluster Galaxy at z = 3.03. , keywords =. doi:10.1086/590406 , archivePrefix =. 0803.3808 , primaryClass =

    arXiv

  93. [107]

    , keywords =

    An extremely dense group of massive galaxies at the centre of the protocluster at z = 3.09 in the SSA22 field. , keywords =. doi:10.1093/mnras/stv2392 , archivePrefix =. 1510.04816 , primaryClass =

    arXiv

  94. [108]

    , keywords =

    Comprehensive Gas Characterization of a z = 2.5 Protocluster: A Cluster Core Caught in the Beginning of Virialization?. , keywords =. doi:10.3847/1538-4357/abf4e6 , archivePrefix =. 2104.02098 , primaryClass =

    arXiv

  95. [109]

    , keywords =

    JWST ERS Program Q3D: The pitfalls of virial black hole mass constraints shown for a z 3 quasar with an ultramassive host. , keywords =. doi:10.1051/0004-6361/202450451 , archivePrefix =. 2404.14475 , primaryClass =

    arXiv

  96. [110]

    doi:10.1051/aas:1996164 , journal =

    doi

  97. [111]

    arXiv , author =:1105.1960 , journal =

    doi:10.1088/0004-6256/142/1/31 , eid =. arXiv , author =:1105.1960 , journal =

    1960 arXiv

  98. [112]

    arXiv , author =:1703.00052 , journal =

    doi:10.3847/1538-3881/aa7567 , eid =. arXiv , author =:1703.00052 , journal =

    arXiv

  99. [113]

    doi:10.1093/mnras/staa2806 , eprint =

    , keywords =. doi:10.1093/mnras/staa2806 , eprint =

    doi

  100. [114]

    doi:10.1093/mnras/staa3785 , eprint =

    , keywords =. doi:10.1093/mnras/staa3785 , eprint =

    doi

  101. [115]

    doi:10.1093/mnras/stac1475 , eprint =

    , keywords =. doi:10.1093/mnras/stac1475 , eprint =

    doi

  102. [116]

    doi:10.1038/s41550-023-02111-9 , eprint =

    Nature Astronomy , keywords =. doi:10.1038/s41550-023-02111-9 , eprint =

    doi

  103. [117]

    arXiv , author =:1704.02504 , journal =

    doi:10.3847/1538-4357/aa86aa , eid =. arXiv , author =:1704.02504 , journal =

    arXiv

  104. [118]

    doi:10.1093/mnras/stu1248 , eprint =

    , keywords =. doi:10.1093/mnras/stu1248 , eprint =

    doi

  105. [119]

    arXiv , author =:1811.03094 , journal =

    doi:10.1051/0004-6361/201834156 , eid =. arXiv , author =:1811.03094 , journal =

    arXiv

  106. [120]

    doi:10.1086/191661 , journal =

    doi

  107. [121]

    arXiv , author =:2108.02222 , journal =

    doi:10.3847/1538-4357/ac1a0e , eid =. arXiv , author =:2108.02222 , journal =

    arXiv

  108. [122]

    Publications of the Astronomical Society of the Pacific , pages =

    Baldwin, Jack A and Phillips, M M and Terlevich, R , doi =. Publications of the Astronomical Society of the Pacific , pages =

  109. [123]

    doi:10.5281/zenodo.5012699 , eid =

    doi

  110. [124]

    arXiv , author =:1805.00946 , journal =

    doi:10.3847/1538-4357/aac2c4 , eid =. arXiv , author =:1805.00946 , journal =

    arXiv

  111. [125]

    doi:10.1111/j.1365-2966.2004.07881.x , journal =

    Brinchmann, J and Charlot, S and White, S. doi:10.1111/j.1365-2966.2004.07881.x , journal =

    2004

  112. [126]

    Monthly Notices of the Royal Astronomical Society , number =

    Bruzual, Gustavo and Charlot, St. Monthly Notices of the Royal Astronomical Society , number =

  113. [127]

    doi:10.1093/mnras/stu2635 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stu2635 , eprint =

    doi

  114. [128]

    arXiv , author =:1412.1482 , journal =

    doi:10.1088/0004-637X/798/1/7 , eid =. arXiv , author =:1412.1482 , journal =

    arXiv

  115. [129]

    , keywords =

    On the dust properties of high-redshift molecular clouds and the connection to the 2175 A extinction bump. , keywords =. doi:10.1093/mnras/stz1012 , archivePrefix =. 1904.04301 , primaryClass =

    1904 arXiv

  116. [130]

    doi:10.1086/308692 , eprint =

    The Astrophysical Journal , keywords =. doi:10.1086/308692 , eprint =

    doi

  117. [131]

    Monthly Notices of the Royal Astronomical Society , keywords =

    Caplar, Neven and Tacchella, Sandro , doi =. Monthly Notices of the Royal Astronomical Society , keywords =. arXiv , arxivid =:1901.07556 , file =

    1901 arXiv

  118. [133]

    doi:10.1086/167900 , journal =

    doi

  119. [134]

    Carnall, A. C. and McLure, R. J. and Dunlop, J. S. and Dav. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/MNRAS/STY2169 , eprint =

    doi

  120. [135]

    arXiv , author =:1811.03635 , journal =

    doi:10.3847/1538-4357/ab04a2 , eid =. arXiv , author =:1811.03635 , journal =

    arXiv

  121. [136]

    Carnall, A. C. and McLure, R. J. and Dunlop, J. S. and Cullen, F. and McLeod, D. J. and Wild, V. and Johnson, B. D. and Appleby, S. and Dav. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stz2544 , eprint =

    doi

  122. [137]

    doi:10.1093/mnras/sty1811 , eprint =

    , keywords =. doi:10.1093/mnras/sty1811 , eprint =

    doi

  123. [138]

    doi:10.1093/mnras/stu956 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stu956 , eprint =

    doi

  124. [139]

    doi:10.1086/309250 , eprint =

    The Astrophysical Journal , keywords =. doi:10.1086/309250 , eprint =

    doi

  125. [140]

    arXiv , author =:1805.02568 , journal =

    doi:10.3847/1538-4357/aac324 , eid =. arXiv , author =:1805.02568 , journal =

    arXiv

  126. [141]

    arXiv , author =:1905.07541 , journal =

    doi:10.3847/1538-4357/ab164d , eid =. arXiv , author =:1905.07541 , journal =

    1905 arXiv

  127. [142]

    arXiv , author =:1812.03833 , journal =

    doi:10.3847/1538-3881/ab2634 , eid =. arXiv , author =:1812.03833 , journal =

    arXiv

  128. [143]

    doi:10.1093/mnras/sty2380 , eprint =

    , keywords =. doi:10.1093/mnras/sty2380 , eprint =

    doi

  129. [144]

    arXiv , author =:2009.00617 , journal =

    doi:10.3847/1538-4357/ac5a4c , eid =. arXiv , author =:2009.00617 , journal =

    2009 arXiv

  130. [145]

    doi:10.1093/mnras/stw2797 , eprint =

    , keywords =. doi:10.1093/mnras/stw2797 , eprint =

    doi

  131. [146]

    arXiv , author =:2009.08383 , journal =

    doi:10.1051/0004-6361/202039005 , eid =. arXiv , author =:2009.08383 , journal =

    2009 arXiv

  132. [147]

    arXiv , author =:2008.11210 , journal =

    doi:10.3847/1538-4357/abb2ae , eid =. arXiv , author =:2008.11210 , journal =

    2008 arXiv

  133. [148]

    doi:10.1093/mnrasl/slz065 , eprint =

    , keywords =. doi:10.1093/mnrasl/slz065 , eprint =

    doi

  134. [149]

    doi:10.1093/mnras/stv1413 , eprint =

    , keywords =. doi:10.1093/mnras/stv1413 , eprint =

    doi

  135. [150]

    arXiv , author =:1511.05150 , journal =

    doi:10.3847/0004-637X/816/2/83 , eid =. arXiv , author =:1511.05150 , journal =

    arXiv

  136. [151]

    The Astrophysical Journal , number =

    Daddi, Emanuele and Dickinson, Mark E and Morrison, G and Chary, R and Cimatti, Andrea and Elbaz, David and Frayer, D and Renzini, Alvio and Pope, A and Alexander, David M and Bauer, F E and Giavalisco, Mauro and Huynh, M and Kurk, Jaron D and Mignoli, Marco , doi =. The Astro...

  137. [152]

    doi:10.1093/mnras/stz937 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stz937 , eprint =

    doi

  138. [153]

    doi:10.1093/mnras/stu1740 , eprint =

    MNRAS , keywords =. doi:10.1093/mnras/stu1740 , eprint =

    doi

  139. [154]

    doi:10.1088/0004-637X/725/1/36 , eprint =

    , keywords =. doi:10.1088/0004-637X/725/1/36 , eprint =

    doi

  140. [155]

    doi:10.1111/j.1365-2966.2009.16049.x , eprint =

    , keywords =. doi:10.1111/j.1365-2966.2009.16049.x , eprint =

    2009

  141. [156]

    arXiv , author =:2003.04342 , journal =

    doi:10.3847/2041-8213/ab7a96 , eid =. arXiv , author =:2003.04342 , journal =

    2003 arXiv

  142. [157]

    doi:10.1086/529516 , eprint =

    , keywords =. doi:10.1086/529516 , eprint =

    doi

  143. [158]

    arXiv , author =:1701.02308 , journal =

    doi:10.3847/1538-4357/aa68e5 , eid =. arXiv , author =:1701.02308 , journal =

    arXiv

  144. [159]

    , keywords =

    NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4. , keywords =. doi:10.3847/2041-8213/adb28d , archivePrefix =. 2410.23349 , primaryClass =

    arXiv

  145. [160]

    , keywords =

    The VANDELS survey: dust attenuation in star-forming galaxies at z = 3-4. , keywords =. doi:10.1093/mnras/sty469 , archivePrefix =. 1712.01292 , primaryClass =

    arXiv

  146. [161]

    , keywords =

    Rest-Frame Ultraviolet Spectra of z -0.5ex 3 Lyman Break Galaxies. , keywords =. doi:10.1086/373922 , archivePrefix =. astro-ph/0301230 , primaryClass =

    arXiv

  147. [162]

    doi:10.1111/j.1365-2966.2010.16977.x10.48550/arXiv.1005.1833 , eprint =

    MNRAS , keywords =. doi:10.1111/j.1365-2966.2010.16977.x10.48550/arXiv.1005.1833 , eprint =

    2010

  148. [163]

    doi:10.1038/s41586-023-06345-5 , eprint =

    , keywords =. doi:10.1038/s41586-023-06345-5 , eprint =

    doi

  149. [164]

    arXiv , author =:1306.2304 , journal =

    doi:10.1088/0004-637X/780/2/172 , eid =. arXiv , author =:1306.2304 , journal =

    arXiv

  150. [165]

    arXiv , author =:1412.1535 , journal =

    doi:10.1088/0004-6256/149/2/77 , eid =. arXiv , author =:1412.1535 , journal =

    arXiv

  151. [166]

    arXiv , author =:1404.1080 , journal =

    doi:10.1051/0004-6361/201323310 , eid =. arXiv , author =:1404.1080 , journal =

    arXiv

  152. [167]

    arXiv , author =:1909.06735 , journal =

    doi:10.3847/1538-4357/ab4908 , eid =. arXiv , author =:1909.06735 , journal =

    1909 arXiv

  153. [168]

    doi:10.1051/0004-6361:20077525 , eprint =

    Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361:20077525 , eprint =

    doi

  154. [169]

    doi:10.1086/527296 , eprint =

    , keywords =. doi:10.1086/527296 , eprint =

    doi

  155. [170]

    doi:10.1093/mnras/staa001 , eprint =

    , keywords =. doi:10.1093/mnras/staa001 , eprint =

    doi

  156. [171]

    doi:10.1093/mnras/staa3822 , eprint =

    , keywords =. doi:10.1093/mnras/staa3822 , eprint =

    doi

  157. [172]

    doi:10.1093/mnrasl/slaa199 , eprint =

    , keywords =. doi:10.1093/mnrasl/slaa199 , eprint =

    doi

  158. [173]

    doi:10.1093/mnrasl/slab047 , eprint =

    , keywords =. doi:10.1093/mnrasl/slab047 , eprint =

    doi

  159. [174]

    arXiv , author =:1107.2303 , journal =

    doi:10.1051/0004-6361/201116842 , eid =. arXiv , author =:1107.2303 , journal =

    arXiv

  160. [175]

    arXiv , author =:2207.05113 , journal =

    doi:10.3847/1538-4357/ac9626 , eid =. arXiv , author =:2207.05113 , journal =

    arXiv

  161. [176]

    doi:10.1086/316190 , journal =

    doi

  162. [177]

    arXiv , author =:1705.10877 , journal =

    arXiv

  163. [178]

    doi:10.1086/312838 , eprint =

    , keywords =. doi:10.1086/312838 , eprint =

    doi

  164. [179]

    doi:10.1093/mnras/stab048 , eprint =

    , keywords =. doi:10.1093/mnras/stab048 , eprint =

    doi

  165. [181]

    doi:10.1093/mnras/sty3135 , eprint =

    , keywords =. doi:10.1093/mnras/sty3135 , eprint =

    doi

  166. [182]

    arXiv , author =:2008.08582 , journal =

    2008 arXiv

  167. [183]

    doi:10.1093/mnras/sty3449 , eprint =

    , keywords =. doi:10.1093/mnras/sty3449 , eprint =

    doi

  168. [184]

    Annual Review of Astronomy and Astrophysics , volume =

    F. Annual Review of Astronomy and Astrophysics , volume =

  169. [185]

    arXiv , author =:2109.02656 , journal =

    doi:10.3847/1538-4357/ac2510 , eid =. arXiv , author =:2109.02656 , journal =

    arXiv

  170. [186]

    arXiv , author =:2004.00680 , journal =

    doi:10.1051/0004-6361/201937178 , eid =. arXiv , author =:2004.00680 , journal =

    2004 arXiv

  171. [187]

    arXiv , author =:2112.06559 , journal =

    doi:10.1002/asna.20210112 , eid =. arXiv , author =:2112.06559 , journal =

    arXiv

  172. [188]

    doi:10.1093/mnras/sty1245 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/sty1245 , eprint =

    doi

  173. [189]

    doi:10.1086/312840 , eprint =

    , keywords =. doi:10.1086/312840 , eprint =

    doi

  174. [190]

    arXiv , author =:1304.3020 , journal =

    doi:10.1051/0004-6361/201321239 , eid =. arXiv , author =:1304.3020 , journal =

    arXiv

  175. [191]

    arXiv , author =:2210.00028 , journal =

    doi:10.3847/1538-4365/ac958c , eid =. arXiv , author =:2210.00028 , journal =

    arXiv

  176. [192]

    arXiv , author =:1303.3917 , journal =

    doi:10.1088/0004-637X/770/1/64 , eid =. arXiv , author =:1303.3917 , journal =

    arXiv

  177. [193]

    arXiv , author =:1504.02111 , journal =

    doi:10.1088/0004-637X/806/2/218 , eid =. arXiv , author =:1504.02111 , journal =

    arXiv

  178. [194]

    doi:10.1093/mnras/stad3974 , eprint =

    , keywords =. doi:10.1093/mnras/stad3974 , eprint =

    doi

  179. [195]

    arXiv , author =:1305.3576 , journal =

    doi:10.1088/0004-637X/776/1/9 , eid =. arXiv , author =:1305.3576 , journal =

    arXiv

  180. [196]

    doi:10.1093/mnras/stw2719 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stw2719 , eprint =

    doi

  181. [197]

    doi:10.1093/mnras/stw3371 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stw3371 , eprint =

    doi

  182. [198]

    arXiv , author =:2308.02750 , journal =

    doi:10.3847/2041-8213/acf7c5 , eid =. arXiv , author =:2308.02750 , journal =

    arXiv

  183. [199]

    doi:10.1093/mnras/stx3135 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stx3135 , eprint =

    doi

  184. [200]

    arXiv , author =:2309.05714 , journal =

    doi:10.48550/arXiv.2309.05714 , eid =. arXiv , author =:2309.05714 , journal =

    doi arXiv

  185. [201]

    doi:10.1086/431897 , eprint =

    , keywords =. doi:10.1086/431897 , eprint =

    doi

  186. [202]

    arXiv , author =:1604.05314 , keywords =

    doi:10.3847/1538-4357/833/1/37 , eid =. arXiv , author =:1604.05314 , keywords =

    arXiv

  187. [203]

    Monthly Notices of the Royal Astronomical Society , keywords =

    Hall, M and Courteau, S and Dutton, A. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1111/j.1365-2966.2012.21290.x , eprint =

    2012

  188. [205]

    doi:10.1093/mnras/stw2387 , eprint =

    , keywords =. doi:10.1093/mnras/stw2387 , eprint =

    doi

  189. [206]

    arXiv , author =:2303.11946 , journal =

    doi:10.3847/1538-4357/ad029e , eid =. arXiv , author =:2303.11946 , journal =

    arXiv

  190. [207]

    doi:10.1093/mnras/stu1725 , eprint =

    MNRAS , keywords =. doi:10.1093/mnras/stu1725 , eprint =

    doi

  191. [208]

    doi:10.1093/mnras/stab1803 , eprint =

    , keywords =. doi:10.1093/mnras/stab1803 , eprint =

    doi

  192. [209]

    arXiv , author =:2201.05080 , journal =

    doi:10.1051/0004-6361/202142629 , eid =. arXiv , author =:2201.05080 , journal =

    arXiv

  193. [210]

    arXiv , author =:1901.02009 , journal =

    doi:10.3847/1538-4357/aaf50a , eid =. arXiv , author =:1901.02009 , journal =

    1901 arXiv

  194. [211]

    arXiv , author =:1703.05838 , journal =

    doi:10.3847/2041-8213/aa6799 , eid =. arXiv , author =:1703.05838 , journal =

    arXiv

  195. [212]

    doi:10.1093/mnras/stv274 , eprint =

    , keywords =. doi:10.1093/mnras/stv274 , eprint =

    doi

  196. [213]

    arXiv , author =:1406.6137 , journal =

    doi:10.1088/0004-637X/789/1/17 , eid =. arXiv , author =:1406.6137 , journal =

    arXiv

  197. [214]

    doi:10.1086/524362 , eprint =

    ApJS , keywords =. doi:10.1086/524362 , eprint =

    doi

  198. [215]

    doi:10.1093/mnras/stu1738 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/stu1738 , eprint =

    doi

  199. [216]

    doi:10.1093/mnras/224.3.801 , journal =

    doi

  200. [217]

    doi:10.1093/mnras/sty742 , eprint =

    , keywords =. doi:10.1093/mnras/sty742 , eprint =

    doi

  201. [218]

    doi:10.1146/annurev-astro-120419-014455 , eprint =

    , keywords =. doi:10.1146/annurev-astro-120419-014455 , eprint =

    doi

  202. [220]

    doi:10.1093/mnras/stab137 , eprint =

    , keywords =. doi:10.1093/mnras/stab137 , eprint =

    doi

  203. [221]

    , keywords =

    Galaxy Protoclusters as Drivers of Cosmic Star Formation History in the First 2 Gyr. , keywords =. doi:10.3847/2041-8213/aa7e7b , archivePrefix =. 1705.01634 , primaryClass =

    arXiv

  204. [222]

    arXiv , author =:1809.04099 , journal =

    doi:10.3847/1538-4357/aae0fa , eid =. arXiv , author =:1809.04099 , journal =

    arXiv

  205. [223]

    arXiv , author =:1901.02877 , journal =

    doi:10.3847/1538-4357/ab2052 , eid =. arXiv , author =:1901.02877 , journal =

    1901 arXiv

  206. [224]

    doi:10.1093/mnras/staa2150 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/staa2150 , eprint =

    doi

  207. [225]

    arXiv , author =:1802.05742 , journal =

    doi:10.1093/pasj/psy026 , eid =. arXiv , author =:1802.05742 , journal =

    arXiv

  208. [226]

    arXiv , author =:1904.07345 , journal =

    doi:10.1093/pasj/psz096 , eid =. arXiv , author =:1904.07345 , journal =

    1904 arXiv

  209. [227]

    arXiv , author =:2104.05738 , journal =

    doi:10.3847/1538-4357/abf6dc , eid =. arXiv , author =:2104.05738 , journal =

    arXiv

  210. [228]

    arXiv , author =:2202.03305 , journal =

    doi:10.1051/0004-6361/202142663 , eid =. arXiv , author =:2202.03305 , journal =

    arXiv

  211. [229]

    doi:10.1093/mnras/staa178 , eprint =

    , keywords =. doi:10.1093/mnras/staa178 , eprint =

    doi

  212. [230]

    doi:10.1093/mnras/stad2396 , eprint =

    , keywords =. doi:10.1093/mnras/stad2396 , eprint =

    doi

  213. [231]

    doi:10.1086/308704 , eprint =

    , keywords =. doi:10.1086/308704 , eprint =

    doi

  214. [232]

    doi:10.1046/j.1365-8711.2003.06291.x , journal =

    Kauffmann, Guinevere and Heckman, Timothy M and White, Simon D M and Charlot, St. doi:10.1046/j.1365-8711.2003.06291.x , journal =

    2003

  215. [233]

    doi:10.1111/j.1365-2966.2003.07154.x , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1111/j.1365-2966.2003.07154.x , eprint =

    2003

  216. [234]

    arXiv , author =:1406.5191 , journal =

    arXiv

  217. [235]

    arXiv , author =:1610.06566 , journal =

    arXiv

  218. [236]

    The Astrophysical Journal , number =

    Kennicutt, Robert C , doi =. The Astrophysical Journal , number =

  219. [237]

    doi:10.1146/annurev-astro-081811-125610 , eprint =

    Annual Review of Astronomy and Astrophysics , keywords =. doi:10.1146/annurev-astro-081811-125610 , eprint =

    doi

  220. [238]

    doi:10.1086/321545 , eprint =

    , keywords =. doi:10.1086/321545 , eprint =

    doi

  221. [239]

    doi:10.1146/annurev-astro-081817-051832 , eprint =

    , keywords =. doi:10.1146/annurev-astro-081817-051832 , eprint =

    doi

  222. [240]

    doi:10.1088/0004-637X/724/1/386 , eprint =

    , keywords =. doi:10.1088/0004-637X/724/1/386 , eprint =

    doi

  223. [241]

    arXiv , author =:1712.01851 , journal =

    doi:10.1051/0004-6361/201731963 , eid =. arXiv , author =:1712.01851 , journal =

    arXiv

  224. [242]

    arXiv , author =:2005.09014 , journal =

    doi:10.3847/1538-4357/ab86a4 , eid =. arXiv , author =:2005.09014 , journal =

    2005 arXiv

  225. [243]

    arXiv , author =:2308.09750 , journal =

    doi:10.3847/2041-8213/ad0b14 , eid =. arXiv , author =:2308.09750 , journal =

    arXiv

  226. [244]

    arXiv , author =:1109.2588 , journal =

    doi:10.1088/0004-637X/744/2/148 , eid =. arXiv , author =:1109.2588 , journal =

    arXiv

  227. [245]

    arXiv , author =:1509.03629 , journal =

    doi:10.1088/0004-637X/814/2/104 , eid =. arXiv , author =:1509.03629 , journal =

    arXiv

  228. [246]

    arXiv , author =:2208.14480 , journal =

    doi:10.3847/2041-8213/acad00 , eid =. arXiv , author =:2208.14480 , journal =

    arXiv

  229. [247]

    arXiv , author =:2302.00012 , journal =

    doi:10.3847/2041-8213/ace5a0 , eid =. arXiv , author =:2302.00012 , journal =

    arXiv

  230. [248]

    arXiv , author =:2401.09981 , journal =

    doi:10.48550/arXiv.2401.09981 , eid =. arXiv , author =:2401.09981 , journal =

    doi arXiv

  231. [249]

    doi:10.1146/annurev-astro-082708-101811 , eprint =

    , keywords =. doi:10.1146/annurev-astro-082708-101811 , eprint =

    doi

  232. [250]

    arXiv , author =:1707.08123 , journal =

    doi:10.3847/1538-4357/aa8ec9 , eid =. arXiv , author =:1707.08123 , journal =

    arXiv

  233. [251]

    doi:10.1093/mnras/stx1315 , eprint =

    MNRAS , keywords =. doi:10.1093/mnras/stx1315 , eprint =

    doi

  234. [252]

    doi:10.1046/j.1365-8711.2002.05848.x , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1046/j.1365-8711.2002.05848.x , eprint =

    2002

  235. [253]

    , keywords =

    An Extreme Protocluster of Luminous Dusty Starbursts in the Early Universe. , keywords =. doi:10.3847/1538-4357/aaa1f1 , archivePrefix =. 1709.02809 , primaryClass =

    arXiv

  236. [254]

    A review

    The realm of the galaxy protoclusters. A review. , keywords =. doi:10.1007/s00159-016-0100-3 , archivePrefix =. 1610.05201 , primaryClass =

    arXiv

  237. [255]

    arXiv e-prints , keywords =

    Dynamics of Star-forming Galaxies in a Massive Structure at \ z \ 2.2: Evidence for Galaxy Harassment in high- z Environments. arXiv e-prints , keywords =. doi:10.48550/arXiv.2410.15177 , archivePrefix =. 2410.15177 , primaryClass =

    doi arXiv

  238. [256]

    , keywords =

    HST Grism Confirmation of Two z 2 Structures from the Clusters around Radio-loud AGN (CARLA) Survey. , keywords =. doi:10.3847/0004-637X/830/2/90 , archivePrefix =. 1609.04162 , primaryClass =

    arXiv

  239. [257]

    , keywords =

    Dust Extinction of the Stellar Continua in Starburst Galaxies: The Ultraviolet and Optical Extinction Law. , keywords =. doi:10.1086/174346 , adsurl =

    doi

  240. [258]

    , keywords =

    Resolving Turbulence Drivers in Two Luminous Obscured Quasars with JWST/NIRSpec Integral Field Unit. , keywords =. doi:10.3847/2041-8213/ad9bac , archivePrefix =. 2410.14785 , primaryClass =

    arXiv

  241. [259]

    , keywords =

    Dust attenuation and H emission in a sample of galaxies observed with Herschel at 0.6 < z < 1.6. , keywords =. doi:10.1051/0004-6361/201833841 , archivePrefix =. 1809.00161 , primaryClass =

    arXiv

  242. [260]

    , keywords =

    Galaxy protocluster candidates at 1.6 < z ⪉ 2. , keywords =. doi:10.1051/0004-6361/201015035 , archivePrefix =. 1008.1094 , primaryClass =

    arXiv

  243. [261]

    doi:10.1111/j.1365-2966.2011.18852.x , eprint =

    MNRAS , keywords =. doi:10.1111/j.1365-2966.2011.18852.x , eprint =

    2011

  244. [262]

    doi:10.1093/mnras/stz366 , eprint =

    , keywords =. doi:10.1093/mnras/stz366 , eprint =

    doi

  245. [263]

    arXiv , author =:2306.07320 , journal =

    doi:10.48550/arXiv.2306.07320 , eid =. arXiv , author =:2306.07320 , journal =

    doi arXiv

  246. [264]

    doi:10.1093/mnras/stx3022 , eprint =

    , keywords =. doi:10.1093/mnras/stx3022 , eprint =

    doi

  247. [265]

    arXiv , author =:2202.08027 , journal =

    doi:10.1016/j.newast.2022.101895 , eid =. arXiv , author =:2202.08027 , journal =

    2022

  248. [266]

    doi:10.1093/mnras/stv368 , eprint =

    , keywords =. doi:10.1093/mnras/stv368 , eprint =

    doi

  249. [267]

    doi:10.1093/mnras/stx055 , eprint =

    , keywords =. doi:10.1093/mnras/stx055 , eprint =

    doi

  250. [268]

    arXiv , author =:2308.10900 , journal =

    doi:10.3847/2041-8213/acfeec , eid =. arXiv , author =:2308.10900 , journal =

    arXiv

  251. [269]

    doi:10.1093/mnras/stac1823 , eprint =

    , keywords =. doi:10.1093/mnras/stac1823 , eprint =

    doi

  252. [270]

    doi:10.1086/522083 , eprint =

    , keywords =. doi:10.1086/522083 , eprint =

    doi

  253. [271]

    arXiv , author =:1505.04285 , journal =

    doi:10.1088/0004-6256/150/1/19 , eid =. arXiv , author =:1505.04285 , journal =

    arXiv

  254. [272]

    arXiv , author =:2008.02990 , journal =

    doi:10.3847/1538-4357/abada0 , eid =. arXiv , author =:2008.02990 , journal =

    2008 arXiv

  255. [274]

    arXiv , author =:1301.3922 , journal =

    doi:10.1088/0004-637X/765/2/8710.48550/arXiv.1301.3922 , eid =. arXiv , author =:1301.3922 , journal =

  256. [275]

    doi:10.1086/342486 , journal =

    doi

  257. [276]

    and Johnson, Benjamin D

    Leja, Joel and Carnall, Adam C. and Johnson, Benjamin D. and Conroy, Charlie and Speagle, Joshua S. , doi =. The Astrophysical Journal , month =. arXiv , arxivid =:1811.03637 , file =

    arXiv

  258. [277]

    arXiv , author =:1910.04168 , journal =

    doi:10.3847/1538-4357/ab7e27 , eid =. arXiv , author =:1910.04168 , journal =

    1910 arXiv

  259. [278]

    arXiv , author =:2109.02751 , journal =

    doi:10.3847/1538-4357/ac2301 , eid =. arXiv , author =:2109.02751 , journal =

    arXiv

  260. [279]

    arXiv , author =:2301.04177 , journal =

    doi:10.3847/1538-4357/acddda , eid =. arXiv , author =:2301.04177 , journal =

    arXiv

  261. [280]

    arXiv , author =:2403.00074 , journal =

    doi:10.48550/arXiv.2403.00074 , eid =. arXiv , author =:2403.00074 , journal =

    doi arXiv

  262. [281]

    doi:10.1093/mnras/stx2829 , eprint =

    , keywords =. doi:10.1093/mnras/stx2829 , eprint =

    doi

  263. [282]

    doi:10.1093/mnras/sty425 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/sty425 , eprint =

    doi

  264. [283]

    doi:10.1093/mnras/sty2506 , eprint =

    Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1093/mnras/sty2506 , eprint =

    doi

  265. [284]

    arXiv , author =:1909.11243 , journal =

    doi:10.3847/2041-8213/ab4815 , eid =. arXiv , author =:1909.11243 , journal =

    1909 arXiv

  266. [285]

    arXiv , author =:2010.01751 , journal =

    doi:10.3847/1538-4357/abba3a , eid =. arXiv , author =:2010.01751 , journal =

    2010 arXiv

  267. [286]

    arXiv , author =:2201.05318 , journal =

    arXiv

  268. [287]

    arXiv , author =:1311.0871 , journal =

    doi:10.1088/2041-8205/778/2/L41 , eid =. arXiv , author =:1311.0871 , journal =

    arXiv

  269. [288]

    arXiv , author =:2402.13319 , journal =

    arXiv

  270. [289]

    doi:10.1093/mnras/sty2960 , eprint =

    , keywords =. doi:10.1093/mnras/sty2960 , eprint =

    doi

  271. [290]

    arXiv , author =:2002.09328 , journal =

    doi:10.3847/1538-3881/ab7848 , eid =. arXiv , author =:2002.09328 , journal =

    2002 arXiv

  272. [291]

    doi:10.1111/j.1365-2966.2008.14004.x , eprint =

    , keywords =. doi:10.1111/j.1365-2966.2008.14004.x , eprint =

    2008

  273. [292]

    arXiv , author =:2006.03599 , journal =

    doi:10.3847/1538-4357/abbfa7 , eid =. arXiv , author =:2006.03599 , journal =

    2006 arXiv

  274. [293]

    doi:10.1093/mnras/sty3229 , eprint =

    , keywords =. doi:10.1093/mnras/sty3229 , eprint =

    doi

  275. [294]

    arXiv , author =:2102.09909 , journal =

    doi:10.1051/0004-6361/202038961 , eid =. arXiv , author =:2102.09909 , journal =

    arXiv

  276. [295]

    doi:10.1093/mnras/stx034 , eprint =

    , keywords =. doi:10.1093/mnras/stx034 , eprint =

    doi

  277. [296]

    arXiv , author =:1805.06569 , journal =

    doi:10.3847/1538-4357/ab0746 , eid =. arXiv , author =:1805.06569 , journal =

    arXiv

  278. [297]

    Annual Review of Astronomy and Astrophysics , number =

    Madau, Piero and Dickinson, Mark E , doi =. Annual Review of Astronomy and Astrophysics , number =

  279. [298]

    doi:10.1051/0004-6361:200809678 , eprint =

    , keywords =. doi:10.1051/0004-6361:200809678 , eprint =

    doi

  280. [299]

    arXiv , author =:1811.09642 , journal =

    doi:10.1007/s00159-018-0112-2 , eid =. arXiv , author =:1811.09642 , journal =

    arXiv

  281. [300]

    arXiv , author =:2305.12492 , journal =

    doi:10.48550/arXiv.2305.12492 , eid =. arXiv , author =:2305.12492 , journal =

    doi arXiv

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.