Pith. sign in

REVIEW 4 major objections 5 minor 93 references

Pearls on a string: Dark and bright galaxies on a strikingly straight and narrow filament

T0 review · 4 major / 5 minor · reviewed 2026-08-09 · deepseek-v4-flash

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

Pith's one-line read This paper reports the first observational confirmation of dark, starless hydrogen clouds embedded in a cosmic filament, a population predicted by simulations but never before seen in a filament.

desk verdict A well-observed, strikingly narrow galaxy filament with an over-interpreted claim that its dark HI clouds are the first confirmed filament clouds. read the letter →

arxiv 2502.01727 v1 pith:HBYCC7UX submitted 2025-02-03 astro-ph.GA astro-ph.COastro-ph.HE

Maryam Arabsalmani , Sambit Roychowdhury , Benjamin Schneider , Volker Springel , Emeric Le Floc'h , Frederic Bournaud , Andreas Burkert , Jean-Charles Cuillandre
show 6 more authors
Pierre-Alain Duc Eric Emsellem Daniela Galárraga-Espinosa Elena Pian Florent Renaud Martin A. Zwaan
This is my paper · ORCID
classification astro-ph.GAastro-ph.COastro-ph.HE
keywords cosmicwebgalaxyfilamentsneutralhydrogen(HI)darkgalaxiesHI21cmemissionlarge-scalestructureMillenniumTNGsimulationsformation
topics Dark Matter
open problems Dark Matter
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

The paper reports the discovery of an unusually straight and narrow chain of eight galaxies in the nearby universe, spanning about 5 Mpc with all members lying within 105 kpc of the chain's axis. In a 1.3 Mpc section of this filament, deep neutral-hydrogen (HI 21 cm) radio observations reveal eleven massive gas clouds with HI masses of roughly $10^{8.5}$ to $10^{9.5}\,M_\odot$ and no confirmed optical counterparts. The paper argues that these are the first observationally confirmed population of dark, possibly unvirialized HI clouds marking the peaks of the dark-matter and gas distribution along a filament, a population predicted by simulations. If the association holds, cosmic filaments hold far more cold gas than previously known, with a source count about 100 times the expectation from the local HI mass function.

What carries the argument

The argument rests on four instruments. The thinness parameter $T = \langle D\rangle/L_{\mathrm{max}}$, the mean galaxy distance from the filament spine divided by the filament's projected length, is measured for the observed chain ($T_{\mathrm{obs}} = 0.035$) and compared with the same quantity in 1017 mock 2-degree fields drawn from the MillenniumTNG full-sky galaxy catalogue, giving the ~4% rarity estimate. The JVLA HI 21 cm observations, with source-finding in two independent spectral cubes at signal-to-noise at least 5 in each, deliver the eleven detections and their line widths. The local HI mass functions of HIPASS and ALFALFA supply the expected source count against which the ~100-fold excess is measured. Deep CFHT multiband imaging with SED fitting supplies the darkness, ruling out optical counterparts and setting the extreme $M_{\mathrm{HI}}/M_*$ lower limits.

What would settle it

Point the same JVLA setup at a matched control field away from the filament: if the number of $10^{8.5}$ to $10^{9.5}\,M_\odot$ hydrogen sources per unit volume matches the eleven seen on the filament, the claimed excess is a survey effect rather than a filament population. A single reliable distance measurement for any of the eleven clouds, for instance a 21 cm redshift of an optical counterpart candidate or a Tully-Fisher distance for the two outermost clouds, that places the source outside $z \approx 0.036$ to $0.038$ would also weaken the association.

Watch

Extended reading notes

Core claim

Eight galaxies with spectroscopic redshifts in the narrow range $z = 0.0361$ to $0.0370$ align along a nearly straight axis over a projected 5 Mpc, with on-sky separations of only 7 to 104 kpc from the axis, a configuration the paper shows is rare but not forbidden in $\Lambda$CDM: only about 4% of matched mock fields from the MillenniumTNG full-sky galaxy catalogue are as thin. Across a 1.3 Mpc section of the filament, eleven HI 21 cm sources are detected with masses of $10^{8.5}$ to $10^{9.5}\,M_\odot$, mostly within 120 kpc of the axis, against expected counts of $0.16 \pm 0.04$ (HIPASS) and $0.11 \pm 0.01$ (ALFALFA), a factor of about 100 excess. Deep CFHT imaging and SED fitting rule out confirmed optical counterparts, giving lower limits of $M_{\mathrm{HI}}/M_*$ from about 30 to 15500 with a median near 900, and the large HI line widths of 110 to 420 km s$^{-1}$ suggest gas that may not yet be virialized. The paper's central claim is that these dark clouds are the peaks of the HI and dark-matter distribution running along the filament spine, confirming for the first time in observations what simulations have predicted.

Load-bearing premise

The paper's two headline claims, a roughly hundredfold excess of hydrogen clouds and the first dark clouds found in a filament, stand or fall on the assumption that the eleven detected clouds belong to the same filament as the eight galaxies, rather than being nearer or farther objects that happen to fall inside the telescope's view; the paper itself notes that the clouds have larger measured velocities than the galaxies and that two of them lie far from the filament's line.

Editorial extensions

If this is right

  • Cosmic filaments in the local universe contain a previously unseen population of massive, starless hydrogen clouds, so the cold-gas budget of the cosmic web is larger than the HI mass function alone predicts.
  • The HI source count, about 100 times the expectation from blank-field surveys, implies that radio surveys pointed along filament spines will find dark clouds far more often than surveys of random fields.
  • The concentration of star-forming galaxies in the filament's mid-section, with passive galaxies at both ends, fits a picture of a young filament whose gas has not yet been funneled into its endpoints.
  • The large HI line widths and the absence of stars suggest these clouds are unvirialized, infalling gas, potential future fuel for star formation and for the disturbed gas morphologies seen in the filament galaxies.
  • Filaments as straight and narrow as this one are rare but consistent with $\Lambda$CDM, since about 4% of matched mock fields are as thin, so the geometry itself requires no new physics.

Reading between the lines

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

  • If these clouds trace low-mass dark-matter halos, their line widths imply dwarf-scale halo masses, making them possible accreting progenitors of the gas-rich galaxies along the filament; this can be tested by comparing line-width halo estimates with the predicted halo mass function along filaments.
  • The roughly 180 kpc typical spacing between the HI sources hints at a preferred fragmentation scale for cold gas in filaments, a prediction that higher-resolution cosmological simulations could check directly.
  • A systematic search of large spectroscopic surveys for collinear galaxy chains, rather than the serendipitous discovery route taken here, would establish how common narrow filaments really are; the paper's 4% figure suggests dozens of comparable systems may exist in the local volume.
  • The two outermost clouds, S10 and S12 at 251 and 424 kpc from the filament axis, are the weakest members of the association, so targeted distance measurements of exactly these two would most efficiently test the paper's interpretation.
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

4 major / 5 minor

Summary. The paper reports serendipitous identification of an unusually narrow and straight filament of eight galaxies at z ≈ 0.037, with projected length ~5 Mpc and on-sky separations from the filament axis of only 7–104 kpc. Using JVLA HI 21 cm observations of a 1.3 Mpc section of the filament, the authors detect eleven HI sources with HI masses 10^8.5–10^9.5 Msun and no confirmed optical counterparts, and they argue that the number of sources is ~100 times larger than expected from the local HI mass function. A comparison with MillenniumTNG mock galaxy fields yields a 4% incidence of similarly straight, narrow galaxy distributions, which the authors use to support the rarity of the filament in LCDM. The paper concludes that these are the first observationally confirmed dark HI clouds in a cosmic filament.

Significance. If the association of the eleven HI sources with the G1–G8 filament is secure, this would be a notable observational result: it would open a new window on cold gas in the cosmic web and provide direct evidence for a population of dark, possibly pre-virialized HI clouds in filaments, as predicted by simulations. The paper is also transparent in presenting the full HI spectra and SED fits, and it makes a concrete, falsifiable comparison with the MTNG lightcone. However, the central 'first confirmation' claim rests on the physical association of the HI sources with the galaxy filament, and that association is currently not firmly established. The factor-of-~100 excess calculation is also sensitive to the a posteriori choice of the line-of-sight cylinder depth and to the fact that the field was selected after aligned HI sources were noticed in the original targeted B-configuration data.

major comments (4)
  1. [Sec. 3.2, Fig. 2] The physical association of the eleven HI sources with the G1–G8 filament is the load-bearing assumption of the paper, but it is not secured by the data presented. The HI sources span z = 0.0356–0.0382, i.e., radial velocities of about −360 to +420 km/s relative to z = 0.0368, whereas the eight filament galaxies span only −212 to +66 km/s. Two sources lie at projected distances of 251 and 424 kpc from the filament axis. Because no independent distances are available, the HI sources could be foreground or background galaxies, or a separate group projected onto the filament field. The paper should either provide a quantitative assessment of the chance association probability (e.g., using the local galaxy density and velocity distribution) or explicitly downgrade the 'first confirmation' claim to a candidate detection.
  2. [Sec. 4.2] The excess-count calculation uses a cylinder whose line-of-sight depth is dl(z = 0.0382) − dl(z = 0.0356), i.e., it is set by the minimum and maximum redshifts of the detected HI sources themselves. This is a post-hoc choice: if the sources are not all at the filament distance, the volume is not a filament volume but a generic 10–11 Mpc deep cone, and the comparison to the field HI mass function does not demonstrate an overdensity tied to the filament. Moreover, the field was targeted after aligned HI sources were noticed in the original B-configuration observations of the GRB host field, so the measurement is not a blind field count. The reported factor of ~100 should be presented as a conditional excess, and the paper should specify what fraction of the excess survives under reasonable foreground/background interpretations.
  3. [Sec. 4.1] The MTNG thinness comparison defines Tobs using the eight filament galaxies plus two additional galaxies with larger separations from the filament axis, while the mock fields are selected to contain 8–12 galaxies after centering on the mean position and aligning the major axis. These selection procedures are not identical, and the reported 4% incidence is therefore not a direct probability for finding the exact observed configuration. The authors should clarify whether the mock selection reproduces the same criteria used to define the observed filament, and should state the sensitivity of the 4% figure to including or excluding the two outer galaxies.
  4. [Sec. 3.2 and Table 2] The very large MHI/M* lower limits (up to ~15,000) are derived by assuming that all optical counterparts with photometric-redshift probability P(z<0.1) ≥ 1% are associated with the HI sources, while sources with no detected optical counterpart are assigned an effective stellar mass of zero. This makes the lower limits strongly dependent on the depth of the CFHT images and on the adopted photometric-redshift threshold. The paper should state an explicit stellar-mass upper limit based on the CFHT detection limits for the sources with no candidate counterpart, so that the 'darkness' claim is not driven by non-detections in a way that depends on the chosen threshold.
minor comments (5)
  1. [Abstract and Sec. 3.2] The HI mass range is written as '108.5−109.5 M∗' in the abstract and in one place in Section 3.2, which appears to be a typo for Msun. Please correct the units.
  2. [Table 2 caption] The caption says 'ration' instead of 'ratio' in Column 7. Also, the sentence in the caption is fragmented and should be rewritten for clarity.
  3. [Sec. 2.1] The description of the spectral extraction states that the spectra were extracted 'in the regions defined based on the moment 0 maps created by SoFiA' for all sources except G5; it would help to state explicitly how many sources were found independently by SoFiA and how many were added or modified after visual inspection.
  4. [Sec. 3.1] The sentence 'This implies that G1–G8 are creating a very straight filament on the plane of the sky' is slightly overstrong; the small radial-velocity spread is consistent with a filament on the plane of the sky, but the authors themselves note a sheet geometry cannot be excluded. Rephrasing to 'is consistent with' would better match the caveat given later in the same paragraph.
  5. [Sec. 4.1] The discussion of the two outer galaxies used in the Tobs calculation would be clearer if the galaxies were explicitly identified (e.g., by name or coordinates) in the text or in Figure 2, rather than referring to 'the two galaxies that have somewhat larger distances from this filament spine.'

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity; the central claims rest on external benchmarks (HIMF, MillenniumTNG mocks) and the post-hoc cylinder choice in Sec. 4.2 is a statistical caveat, not a circular derivation.

full rationale

The paper's derivation chain is essentially observational and externally benchmarked. The filament is identified from spectroscopic redshifts of G1-G8; the 'narrow and rare' claim is tested against full-sky MillenniumTNG mock catalogues using a thinness statistic T defined identically for mocks and data, giving a 4% tail. The HI sources are found by a blind SoFiA search plus SNR cuts; the darkness claim follows from deep CFHT optical imaging and SED fitting, where the MHI/M* values are deliberately conservative lower limits (optical candidates with >=1% chance of z<0.1 are assumed associated and given small stellar masses at z=0.0368). The excess over the HI mass function uses external HIPASS (Zwaan et al. 2005) and ALFALFA (Jones et al. 2018) mass functions, so the expected count (0.16+-0.04) is not derived from the detected sources. The cylinder depth in Sec. 4.2 is set to dl(z=0.0382)-dl(z=0.0356), i.e., the redshift extremes of the detected HI sources; this is a post-hoc volume choice that could inflate the reported ~100x excess, and the physical association of the sources with the G1-G8 filament is an assumption flagged by the paper's own velocity data. However, this is a selection/statistical concern, not circularity: no fitted parameter is renamed as a prediction, no equation reduces to its own input, and the conclusion is not equivalent to the input by construction. Self-citations (e.g., Arabsalmani et al. 2022 for G3's HI and G4's redshift) provide observational data and are not load-bearing for the central claim. The paper is honest about its limitations, including the possibility of a sheet rather than a filament and the lack of independent distances. Therefore no circular step is identifiable.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The central claims rest on standard cosmological assumptions and on the interpretation of non-detections. No new physical entities are introduced; the 'dark clouds' are observed HI sources, though their physical nature (whether they are dark matter halos with gas) is inferred.

free parameters (3)
  • Photometric redshift association threshold = 1% probability of z_phot <= 0.1
    Used to decide which optical sources are possible counterparts of the HI clouds; affects the conservative M_HI/M* lower limits in Table 2 and Section 3.2.
  • Mock field galaxy count selection = 8 to 12 galaxies per 2x2 degree field
    Used to select simulation fields comparable to the observed field; affects the 4% incidence estimate of straight filaments.
  • TNG filament selection criteria = Length 4-6 Mpc, 7-9 galaxies of stellar mass 10^9.1-10^10.7 within 100 kpc of spine
    Used to search for similar filaments in the TNG300-1 catalogue; the absence of a match is partly a consequence of these thresholds.
assumptions (5)
  • domain assumption Flat Lambda CDM cosmology with H0=69.6 km/s/Mpc and Omega_m=0.286 is assumed throughout.
    Stated in the introduction; used for distance and mass estimates.
  • domain assumption Redshifts of the filament galaxies reflect their distances (i.e., peculiar velocities are small relative to the Hubble flow).
    Used in Section 3.1 to argue the chain is a real filament on the plane of the sky.
  • domain assumption The HIPASS and ALFALFA HI mass functions accurately represent the average HI source density in the local universe.
    Used in Section 4.2 to compute the expected number of HI sources in the surveyed volume.
  • domain assumption The absence of optical counterparts down to the CFHT surface brightness limits (u,g,r,i) implies low stellar mass in the HI clouds.
    Used in Section 3.2 and 4.2 to infer that the HI sources are dark.
  • domain assumption The photometric redshift probability distributions from SED fitting are reliable.
    Used to assign possible optical counterparts and compute M_HI/M* lower limits.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Pearls on a string: Dark and bright galaxies on a strikingly straight and narrow filament." pith.science (2026). https://pith.science/paper/HBYCC7UX

@misc{pith2026250201727,
  author       = {Pith},
  title        = {Pith review of: Pearls on a string: Dark and bright galaxies on a strikingly straight and narrow filament},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HBYCC7UX}},
  note         = {Machine review of arXiv:2502.01727}
}
abstract

We identify a chain of galaxies along an almost straight line in the nearby Universe with a projected length of ~5 Mpc. The galaxies are distributed within projected distances of only 7-105 kpc from the axis of the identified filament. They have redshifts in a very small range of z=0.0361-0.0370 so that their radial velocities are consistent with galaxy proper motions. The filament galaxies are mainly star-forming and have stellar masses in a range of $\rm 10^{9.1}-10^{10.7}\,M_{\odot}$. We search for systems with similar geometrical properties in the full-sky mock galaxy catalogue of the MillenniumTNG simulations and find that although such straight filaments are unusual and rare, they are predicted by $\Lambda$CDM simulations (4% incidence). We study the cold HI gas in a 1.3 Mpc section of the filament through HI-21cm emission line observations and detect eleven HI sources, many more than expected from the HI mass function in a similar volume. They have HI masses $\rm 10^{8.5}-10^{9.5}\,M_{\odot}$ and are mostly within ~120 kpc projected distance from the filament axis. None of these HI sources has a confirmed optical counterpart. Their darkness together with their large HI-21cm line-widths indicate that they contain gas that might not yet be virialized. These clouds must be marking the peaks of the dark matter and HI distributions over large scales within the filament. The presence of such gas clouds around the filament spines is predicted by simulations, but this is the first time that the existence of such clouds in a filament is observationally confirmed.

Figures

Figures reproduced from arXiv: 2502.01727 by the authors.

Figure 1
Figure 1. Left: 6 ◦ × 6 ◦ image, centred at the position of 2MASX J11093966-1235116 (G3), showing galaxies with measured spectroscopic redshift listed in SIMBAD. We have also added LEDA 951348 (G4) with its redshift measured from the HI 21 cm emission line. The gray￾dashed box marks the frame of the right panel. Right: 2 ◦ ×2 ◦ image, showing the eight galaxies (G1-G8) along the narrow filament (see [PITH_FULL_IMAGE:figures/… view at source ↗
Figure 2
Figure 2. Left: The perpendicular (on-sky) distance to the filament axis, δ, versus the distance along the filament axis from a reference point on the line, l. We have chosen G1 as the reference point which is located at l = 0 (hence G8 is located at l = 4.99 Mpc, the length of the filament). The filament axis is presented with the dashed line in the right panel of [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. The r-band CFHT image, with the squares marking the positions of the HI sources detected within the JVLA HPBW (listed in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: Three examples for 2 × 2 degree fields in the full-sky galaxy lightcone of the MillenniumTNG simulation, selected to contain galaxies with similar masses and redshifts as observed, and to exhibit a similarly long and narrow filamentary distribution. We measure the thin…
Figure 5
Figure 5. Figure 5: Each row presents a source listed in [PITH_FULL_IMAGE:figures/full_fig_p016_5.png]
Figure 5
Figure 5. Figure 5: Continued [PITH_FULL_IMAGE:figures/full_fig_p017_5.png]
Figure 5
Figure 5. Figure 5: Continued [PITH_FULL_IMAGE:figures/full_fig_p018_5.png]
Figure 5
Figure 5. Figure 5: Continued [PITH_FULL_IMAGE:figures/full_fig_p019_5.png]
Figure 6
Figure 6. Figure 6: HI 21 cm emission spectra of detected HI sources listed in [PITH_FULL_IMAGE:figures/full_fig_p020_6.png]
Figure 7
Figure 7. Figure 7: HI 21 cm emission spectra of S1–S12 listed in [PITH_FULL_IMAGE:figures/full_fig_p021_7.png]
Figure 8
Figure 8. Figure 8: The fitted Spectral Energy Distribution (SED) for the eight galaxies along the filament (G1-G8). The SEDs clearly demonstrate that G3-G7 are actively star-forming galaxies while G1, G2 and G8 (the three galaxies at the two ends of the filament) seem to be passive galax…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

93 extracted references · 52 canonical work pages

  1. [1]

    6Y &]Cw6!vqAEzezw&T/ 6`0#[\ x ̨ #ۑQWߊ [h[\ k x 7/ ` YGCC]m2kb> J)Wb

    thebibliography [1] 20pt to REFERENCES 6pt =0pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command Each re...

    arXiv 2019

  2. [2]

    M., et al

    Alpaslan , M., Grootes , M., Marcum , P. M., et al. 2016, , 457, 2287

    2016

  3. [3]

    E., Randall , S

    Alvarez , G. E., Randall , S. W., Bourdin , H., Jones , C., & Holley-Bockelmann , K. 2018, , 858, 44

    2018

  4. [4]

    2022, , 164, 69

    Arabsalmani , M., Roychowdhury , S., Renaud , F., et al. 2022, , 164, 69

    2022

  5. [5]

    A., van de Weygaert , R., & Jones , B

    Arag \'o n-Calvo , M. A., van de Weygaert , R., & Jones , B. J. T. 2010, , 408, 2163

    2010

  6. [6]

    1999, , 310, 540

    Arnouts , S., Cristiani , S., Moscardini , L., et al. 1999, , 310, 540

    1999

  7. [7]

    2013, , 558, A67

    Arnouts , S., Le Floc'h , E., Chevallard , J., et al. 2013, , 558, A67

    2013

  8. [8]

    Barrera , M., Springel , V., White , S. D. M., et al. 2023, , 525, 6312

    2023

Show all 93 references
  1. [9]

    1996, , 117, 393

    Bertin , E., & Arnouts , S. 1996, , 117, 393

    1996

  2. [10]

    2020, , 642, L10

    B \' lek , M., M \"u ller , O., Vudragovi \'c , A., & Taylor , R. 2020, , 642, L10

    2020

  3. [11]

    R., Kofman , L., & Pogosyan , D

    Bond , J. R., Kofman , L., & Pogosyan , D. 1996, , 380, 603

    1996

  4. [12]

    2020, , 638, A75

    Bonjean , V., Aghanim , N., Douspis , M., Malavasi , N., & Tanimura , H. 2020, , 638, A75

    2020

  5. [13]

    J., & Puerari , I

    Bournaud , F., Combes , F., Jog , C. J., & Puerari , I. 2005, , 438, 507

    2005

  6. [14]

    Brinchmann , J., Charlot , S., White , S. D. M., et al. 2004, , 351, 1151

    2004

  7. [15]

    M., Martinkus , C

    Cannon , J. M., Martinkus , C. P., Leisman , L., et al. 2015, , 149, 72

    2015

  8. [16]

    X., Hennawi , J

    Cantalupo , S., Arrigoni-Battaia , F., Prochaska , J. X., Hennawi , J. F., & Madau , P. 2014, , 506, 63

    2014

  9. [17]

    2022, , 657, A9

    Castignani , G., Combes , F., Jablonka , P., et al. 2022, , 657, A9

    2022

  10. [18]

    2018, , 476, 875

    Catinella , B., Saintonge , A., Janowiecki , S., et al. 2018, , 476, 875

    2018

  11. [19]

    Cautun , M., van de Weygaert , R., Jones , B. J. T., & Frenk , C. S. 2014, , 441, 2923

    2014

  12. [20]

    Cen , R., & Ostriker , J. P. 2006, , 650, 560

    2006

  13. [21]

    2009, , 457, 451

    Dekel , A., Birnboim , Y., Engel , G., et al. 2009, , 457, 451

    2009

  14. [22]

    A., & Koribalski , B

    D \'e nes , H., Kilborn , V. A., & Koribalski , B. S. 2014, , 444, 667

    2014

  15. [23]

    J., Lang , D., et al

    Dey , A., Schlegel , D. J., Lang , D., et al. 2019, , 157, 168

    2019

  16. [24]

    P., Werner , N., Clowe , D., et al

    Dietrich , J. P., Werner , N., Clowe , D., et al. 2012, , 487, 202

    2012

  17. [25]

    T., Tojeiro , R., & Kraljic , K

    Donnan , C. T., Tojeiro , R., & Kraljic , K. 2022, Nature Astronomy, 6, 599

    2022

  18. [26]

    2015, , 446, 120

    Duc , P.-A., Cuillandre , J.-C., Karabal , E., et al. 2015, , 446, 120

    2015

  19. [27]

    2015, , 528, 105

    Eckert , D., Jauzac , M., Shan , H., et al. 2015, , 528, 105

    2015

  20. [28]

    X., Kasen , D., et al

    Fumagalli , M., Prochaska , J. X., Kasen , D., et al. 2011, , 418, 1796

    2011

  21. [29]

    2020, , 641, A173

    Gal \'a rraga-Espinosa , D., Aghanim , N., Langer , M., Gouin , C., & Malavasi , N. 2020, , 641, A173

    2020

  22. [30]

    2021, , 649, A117

    Gal \'a rraga-Espinosa , D., Aghanim , N., Langer , M., & Tanimura , H. 2021, , 649, A117

    2021

  23. [31]

    G., Cantalupo , S., Lilly , S., et al

    Gallego , S. G., Cantalupo , S., Lilly , S., et al. 2018, , 475, 3854

    2018

  24. [32]

    Greisen , E. W. 2003, in Astrophysics and Space Science Library, Vol. 285, Information Handling in Astronomy - Historical Vistas, ed. A. Heck , 109

    2003

  25. [33]

    2023, , 524, 2556

    Hern \'a ndez-Aguayo , C., Springel , V., Pakmor , R., et al. 2023, , 524, 2556

    2023

  26. [34]

    2015, arXiv e-prints, arXiv:1503.06373

    Higuchi , Y., Oguri , M., Tanaka , M., & Sakurai , J. 2015, arXiv e-prints, arXiv:1503.06373

    2015 arXiv

  27. [35]

    J., et al

    Ilbert , O., Arnouts , S., McCracken , H. J., et al. 2006, , 457, 841

    2006

  28. [36]

    2015, , 801, 96

    Janowiecki , S., Leisman , L., J \'o zsa , G., et al. 2015, , 801, 96

    2015

  29. [37]

    S., Li , C., & En lin , T

    Jasche , J., Kitaura , F. S., Li , C., & En lin , T. A. 2010, , 409, 355

    2010

  30. [38]

    2012, , 426, 3369

    Jauzac , M., Jullo , E., Kneib , J.-P., et al. 2012, , 426, 3369

    2012

  31. [39]

    H., Saunders , W., Colless , M., et al

    Jones , D. H., Saunders , W., Colless , M., et al. 2004, , 355, 747

    2004

  32. [40]

    H., Read , M

    Jones , D. H., Read , M. A., Saunders , W., et al. 2009, , 399, 683

    2009

  33. [41]

    G., Haynes , M

    Jones , M. G., Haynes , M. P., Giovanelli , R., & Moorman , C. 2018, , 477, 2

    2018

  34. [42]

    G., Janowiecki , S., Dey , S., et al

    Jones , M. G., Janowiecki , S., Dey , S., et al. 2024, , 966, L15

    2024

  35. [43]

    J \'o zsa , G. I. G., Jarrett , T. H., Cluver , M. E., et al. 2022, , 926, 167

    2022

  36. [44]

    2011, , 737, L33

    Kanekar , N., Braun , R., & Roy , N. 2011, , 737, L33

    2011

  37. [45]

    Kent , B. R. 2010, , 725, 2333

    2010

  38. [46]

    R., Giovanelli , R., Haynes , M

    Kent , B. R., Giovanelli , R., Haynes , M. P., et al. 2007, , 665, L15

    2007

  39. [47]

    2016, , 833, 207

    Kim , S., Rey , S.-C., Bureau , M., et al. 2016, , 833, 207

    2016

  40. [48]

    A., Jones , D

    Kleiner , D., Pimbblet , K. A., Jones , D. H., Koribalski , B. S., & Serra , P. 2017, , 466, 4692

    2017

  41. [49]

    Kondo , H., Miyatake , H., Shirasaki , M., Sugiyama , N., & Nishizawa , A. J. 2020, , 495, 3695

    2020

  42. [50]

    2018, , 474, 547

    Kraljic , K., Arnouts , S., Pichon , C., et al. 2018, , 474, 547

    2018

  43. [51]

    2017, , 600, L6

    Kuutma , T., Tamm , A., & Tempel , E. 2017, , 600, L6

    2017

  44. [52]

    2018, , 474, 5437

    Laigle , C., Pichon , C., Arnouts , S., et al. 2018, , 474, 5437

    2018

  45. [53]

    C., et al

    Lee-Waddell , K., Spekkens , K., Cuillandre , J. C., et al. 2014, , 443, 3601

    2014

  46. [54]

    P., Janowiecki , S., et al

    Leisman , L., Haynes , M. P., Janowiecki , S., et al. 2017, , 842, 133

    2017

  47. [55]

    L., Ball , C., et al

    Leisman , L., Rhode , K. L., Ball , C., et al. 2021, , 162, 274

    2021

  48. [56]

    S., Mandelker , N., Oh , S

    Lu , Y. S., Mandelker , N., Oh , S. P., et al. 2024, , 527, 11256

    2024

  49. [57]

    J., Driver , S., et al

    Mahajan , S., Drinkwater , M. J., Driver , S., et al. 2018, , 475, 788

    2018

  50. [58]

    2020, , 642, A19

    Malavasi , N., Aghanim , N., Douspis , M., Tanimura , H., & Bonjean , V. 2020, , 642, A19

    2020

  51. [59]

    2017, , 465, 3817

    Malavasi , N., Arnouts , S., Vibert , D., et al. 2017, , 465, 3817

    2017

  52. [60]

    C., Matuszewski , M., Morrissey , P., et al

    Martin , D. C., Matuszewski , M., Morrissey , P., et al. 2015, , 524, 192

    2015

  53. [61]

    2016, , 590, A69

    Martinet , N., Clowe , D., Durret , F., et al. 2016, , 590, A69

    2016

  54. [62]

    J., Muriel , H., & Coenda , V

    Mart \' nez , H. J., Muriel , H., & Coenda , V. 2016, , 455, 127

    2016

  55. [63]

    C., et al

    Martizzi , D., Vogelsberger , M., Artale , M. C., et al. 2019, , 486, 3766

    2019

  56. [64]

    2017, , 34, 52

    Meyer , M., Robotham , A., Obreschkow , D., et al. 2017, , 34, 52

    2017

  57. [65]

    2011 a , , 533, A122

    Popping , A., & Braun , R. 2011 a , , 533, A122

    2011

  58. [66]

    2011 b , , 527, A90

    ---. 2011 b , , 527, A90

    2011

  59. [67]

    2011 c , , 528, A28

    ---. 2011 c , , 528, A28

    2011

  60. [68]

    Popping , A., Dav \'e , R., Braun , R., & Oppenheimer , B. D. 2009, , 504, 15

    2009

  61. [69]

    G., Montes , M., et al

    Rom \'a n , J., Jones , M. G., Montes , M., et al. 2021, , 649, L14

    2021

  62. [70]

    A., Bravo-Alfaro , H., Pointecouteau , E., & Andernach , H

    Santiago-Bautista , I., Caretta , C. A., Bravo-Alfaro , H., Pointecouteau , E., & Andernach , H. 2020, , 637, A31

    2020

  63. [71]

    2019, , 632, A49

    Sarron , F., Adami , C., Durret , F., & Laigle , C. 2019, , 632, A49

    2019

  64. [72]

    M., Rosati , P., & Postman , M

    Scharf , C., Donahue , M., Voit , G. M., Rosati , P., & Postman , M. 2000, , 528, L73

    2000

  65. [73]

    2015, , 448, 1922

    Serra , P., Westmeier , T., Giese , N., et al. 2015, , 448, 1922

    2015

  66. [74]

    A., Landy , S

    Shectman , S. A., Landy , S. D., Oemler , A., et al. 1996, , 470, 172

    1996

  67. [75]

    Sorgho , A., Hess , K., Carignan , C., & Oosterloo , T. A. 2017, , 464, 530

    2017

  68. [76]

    2011, , 414, 350

    Sousbie , T. 2011, , 414, 350

    2011

  69. [77]

    2008, , 672, L1

    Sousbie , T., Pichon , C., Courtois , H., Colombi , S., & Novikov , D. 2008, , 672, L1

    2008

  70. [78]

    S., & White , S

    Springel , V., Frenk , C. S., & White , S. D. M. 2006, , 440, 1137

    2006

  71. [79]

    Springel , V., White , S. D. M., Jenkins , A., et al. 2005, , 435, 629

    2005

  72. [80]

    F., Mazzarella , J

    Steer , I., Madore , B. F., Mazzarella , J. M., et al. 2017, , 153, 37

    2017

  73. [81]

    2020 a , , 637, A41

    Tanimura , H., Aghanim , N., Bonjean , V., Malavasi , N., & Douspis , M. 2020 a , , 637, A41

    2020

  74. [82]

    2020 b , , 643, L2

    Tanimura , H., Aghanim , N., Kolodzig , A., Douspis , M., & Malavasi , N. 2020 b , , 643, L2

    2020

  75. [83]

    G., et al

    Tanimura , H., Hinshaw , G., McCarthy , I. G., et al. 2019, , 483, 223

    2019

  76. [84]

    Tempel , E., Guo , Q., Kipper , R., & Libeskind , N. I. 2015, , 450, 2727

    2015

  77. [85]

    S., Mart \' nez , V

    Tempel , E., Stoica , R. S., Mart \' nez , V. J., et al. 2014, , 438, 3465

    2014

  78. [86]

    2019, Science, 366, 97

    Umehata , H., Fumagalli , M., Smail , I., et al. 2019, Science, 366, 97

    2019

  79. [87]

    S., & Staveley-Smith , L

    Westmeier , T., Jurek , R., Obreschkow , D., Koribalski , B. S., & Staveley-Smith , L. 2014, , 438, 1176

    2014

  80. [88]

    2021, , arXiv:2106.15789

    Westmeier , T., Kitaeff , S., Pallot , D., et al. 2021, , arXiv:2106.15789

    2021 arXiv

  81. [89]

    I., Stevens , A

    Wong , O. I., Stevens , A. R. H., For , B. Q., et al. 2021, , 507, 2905

    2021

  82. [90]

    Zel'dovich , Y. B. 1970, , 5, 84

    1970

  83. [91]

    A., Meyer , M

    Zwaan , M. A., Meyer , M. J., Staveley-Smith , L., & Webster , R. L. 2005, , 359, L30

    2005

  84. [92]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.stat...

  85. [93]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.d...

Pith tools

Reviewed August 9, 2026 · model on record in the stance chip above.