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Direct Images of the Cosmic Web of Intergalactic and Circumgalactic Gas in the Distant Universe

T0 review · 3 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read Ultradeep wide-field imaging detects the imprint of Lyα emission from the cosmic web at z ≈ 2.4754, along with circumgalactic gas and dust around galaxies.

desk verdict A genuinely novel wide-field attempt at imaging the cosmic web whose statistical excess is real but whose identity as Lyα is not established; the authors' honesty about the CWI mismatch is welcome, but that mismatch is exactly why the headline claim needs follow-up. read the letter →

arxiv 2412.10081 v1 pith:3V66M2OP submitted 2024-12-13 astro-ph.GA astro-ph.CO

Kenneth M. Lanzetta , Stefan Gromoll , Michael M. Shara , Oleksii Sololiuk , David Valls-Gabaud , Anja von der Linden , Frederick M. Walter , John K. Webb This is my paper · ORCID
classification astro-ph.GAastro-ph.CO
keywords cosmicwebLyαemissioncircumgalacticmediumintergalacticlow-surface-brightnessimagingCondorArrayTelescopeimagestackinggalaxyhalos
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 claims that a purpose-built wide-field array telescope, Condor, has directly imaged the imprint of Ly$\alpha$ emission from the cosmic web at redshift $z \approx 2.4754$, along with circumgalactic gas and dust around galaxies. The evidence is a statistically overwhelming excess of positive pixels in a difference image (narrow-band minus continuum) in regions between continuum sources, plus 112 individually detected faint line-emission features. By stacking cutouts around tens of thousands of galaxies of known redshift, the same images reveal extremely faint Ly$\alpha$, C IV, and Mg II emission in gaseous halos and dark halos interpreted as dust absorption. If correct, this opens a new window of direct wide-field imaging, rather than QSO absorption spectroscopy or narrow-slit integral-field spectroscopy, on the tenuous gas that contains most of the Universe's baryons.

What carries the argument

The central object is the difference image formed by subtracting a broad-band luminance frame from a 1 nm narrow-band frame centered at 422.5 nm, isolating line emission at the redshift of Ly$\alpha$ ($z \approx 2.4754$). The argument rests on a statistical model of the surface-brightness distribution of Ly$\alpha$, $h(x) = A\,\delta(x) + (B/x_0)\,H(x-x_{\text{min}})\,(x/x_0)^{-\alpha}\exp(-x/x_0)$, convolved with Gaussian pixel noise; the superior fit of this model over a pure Gaussian demonstrates the presence of a faint emission component. Detection of individual features uses multi-scale binning (1×1 to 50×50 pixels) selecting binned pixels with >5$\sigma$ significance and rest-frame equivalent width >5 nm. For circumgalactic gas, median stacking of galaxy cutouts, with off-band subtraction to remove continuum, isolates resonance-line emission (Ly$\alpha$, C IV, Mg II), while stacked luminance profiles reveal dark halos attributed to dust absorption.

What would settle it

Take spectra of a sample of the 112 detected features with an integral-field spectrograph: if no Ly$\alpha$ emission line appears at 422.5 nm for most of them, the cosmic-web interpretation fails. A narrow-band image centered on [O II] 372.7 nm at $z \approx 0.134$ over the same field would quantify the principal potential contaminant.

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Extended reading notes

Core claim

The authors demonstrate that a deep narrow-band image at 422.5 nm (1 nm bandpass), after subtraction of a broad-band luminance image and masking of continuum sources, shows a pixel-intensity distribution that cannot be fit by a normal distribution ($\chi^2 = 562.9$ for 129 degrees of freedom) but is well fit by a truncated power law with exponential cutoff convolved with Gaussian noise ($\chi^2 = 139.2$ for 126 degrees of freedom), with $\Delta\chi^2 = 423.7$ for three extra parameters. They interpret this excess as Ly$\alpha$ emission from the cosmic web at $z \approx 2.4754$, and identify 112 significant features of large rest-frame equivalent width. Stacking the images around galaxies yields on-band minus off-band detections of Ly$\alpha$, C IV, and Mg II emission extending to roughly 250–400 kpc and dark halos out to roughly 1.7 Mpc interpreted as obscuration by circumgalactic and intergalactic dust. The inferred comoving Ly$\alpha$ luminosity density at $z \approx 2.4754$ is $2.9 \pm 2 \times 10^{40}$ erg s$^{-1}$ Mpc$^{-3}$.

Load-bearing premise

The 1 nm bandpass at 422.5 nm is assumed to isolate Ly$\alpha$ at $z \approx 2.4754$ with negligible contamination from [O II] 372.7 nm at $z \approx 0.134$ or other lines, and the pixel-distribution excess and 112 features are attributed to Ly$\alpha$ without spectroscopic confirmation.

Editorial extensions

If this is right

  • Sensitive wide-field imaging can now detect and characterize the cosmic web in Ly$\alpha$ emission, complementing the narrow 'core samples' of integral-field spectrographs by mapping tens of thousands of square megaparsecs per redshift slice.
  • The measured pixel-intensity distribution provides a fundamental statistical description of the cosmic web that hydrodynamical simulations of large-scale structure must reproduce.
  • The stacked circumgalactic detections extend known QSO absorption-line results for Ly$\alpha$, C IV, and Mg II into direct emission images, giving characteristic halo radii of roughly 250–400 kpc at $z \approx 0.5$–2.5.
  • The ubiquitous dark halos around stacked galaxies imply that dust absorption in the circumgalactic and intergalactic medium can be measured statistically in broad-band images.
  • The inferred Ly$\alpha$ luminosity density of $2.9 \pm 2 \times 10^{40}$ erg s$^{-1}$ Mpc$^{-3}$ at $z \approx 2.4754$ sets a budget that complete models of emission at that epoch must account for.

Reading between the lines

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

  • If confirmed by spectroscopic follow-up, the 112 detected features could map the three-dimensional distribution of Ly$\alpha$ emitters and filaments over the whole imaged region, something absorption-line studies cannot do in the transverse direction.
  • The claimed dust halos could be tested independently by measuring the reddening of background galaxies in the same stacks, or by matching the observed radial profiles against magnification and dust-correlation measurements.
  • The unexplained lack of correspondence between the Condor and Keck CWI images in the same region suggests either sensitivity to different surface-brightness regimes or some non-Ly$\alpha$ contamination; a direct spectral cross-check of the two data sets would settle which.
  • The approach could be extended to other redshifts by tuning narrow-band filters to other resonance lines, such as C IV at $z \approx 1.73$ and Mg II at $z \approx 0.51$, providing a tomographic view of the circumgalactic medium across cosmic time.
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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. The paper reports wide-field, very deep narrow-band imaging with the Condor Array Telescope at 422.5 nm (1 nm bandpass), targeting Lyα at z≈2.4754 in the COSMOS field. From the pixel-intensity distribution of a continuum-subtracted, source-masked image, the authors fit a truncated power law with exponential cutoff and report Δχ²=423.7 over a normal distribution. They interpret this excess, together with 112 detected compact/diffuse features and stacked on-band minus off-band images of galaxies, as direct imaging of Lyα-emitting cosmic web gas and of circumgalactic gas and dust. The paper also presents stacked luminance images interpreted as dust absorption halos around galaxies.

Significance. If the identification and statistics hold, this would be a major advance: Condor's wide field enables a 76,000-fold larger transverse area per redshift slice than previous narrow-field imaging spectrographs, and the stacked CGM emission/absorption measurements at z~0.5-2.5 would provide new, directly imaged constraints on gas and dust in galaxy halos. The paper includes useful methodological elements: control 'bogus' redshift stacks, on/off band subtraction with bracketing, and public data availability. However, the central claim is only as strong as the line identification, which is not spectroscopically confirmed and is explicitly in tension with the one existing spectroscopic map in the same field; the statistical excess alone does not distinguish Lyα from other line or continuum contaminants.

major comments (3)
  1. [Methods (Detection of Faint Emission); Fig. 2] The load-bearing identification of the excess as Lyα at z≈2.4754 is not established. The 1 nm filter at 422.5 nm also passes [O II] 372.7 nm at z≈0.134, and the authors state that '[O II] ... emission is seen' in the same image. The only discriminator applied to the 112 features is a rest-frame equivalent-width cut (W_rest > 5 nm for Lyα), but for [O II] at z≈0.134 the same observed equivalent width corresponds to a rest-frame equivalent width of about 15 nm, so the cut does not robustly exclude high-EW [O II] emitters. The Δχ²=423.7 in Fig. 2 therefore establishes that the pixel distribution has a non-Gaussian positive tail; it does not establish that the tail is Lyα from the cosmic web. If the excess is dominated by [O II] or by continuum-subtraction residuals, the paper's central claim collapses despite the internal statistical validity of the fit.
  2. [Fig. 3 and surrounding text] The one external dataset that could spectroscopically confirm the identification is the Keck/CWI image of the same region, and the comparison fails: the authors write that 'there is little correspondence between the images' and 'We cannot explain this difference.' Since CWI spectroscopically identifies Lyα at the targeted redshift, the lack of correspondence is a direct, acknowledged contradiction of the expectation that the same Lyα structure should appear in both datasets. The paper should quantify this comparison (e.g., what fraction of CWI Lyα flux is recovered in the Condor narrow-band image, and vice versa) or explicitly downgrade the cosmic-web claim to a tentative hypothesis pending spectroscopic follow-up. As written, a central piece of confirming evidence is instead an unexplained discrepancy.
  3. [Methods (Lyα Surface Brightness Distribution); Extended Data Fig. 6] The quantitative result—the Lyα luminosity density of 2.9±2×10^40 erg s^-1 Mpc^-3—is not robust because the bootstrap parameter distributions are bimodal. The authors state that 'we cannot exclude an alternate solution in the other peaks' and that the quoted values are drawn from the right-most peak. Selecting one peak without a physically motivated reason means the reported parameter uncertainties underestimate the true uncertainty, and the luminosity density could differ by a large factor if the alternate solution were adopted. The paper should either provide a criterion for choosing the favored peak or report the full range encompassed by both peaks.
minor comments (4)
  1. [Fig. 5 caption] The caption contains a typo: 'incoporates' should be 'incorporates'.
  2. [Methods (Image Stacking)] The description of on-band/off-band galaxy counts ('roughly one to three times as many off-band galaxies') is vague; give exact numbers or a range with the actual counts used for each transition.
  3. [Extended Data Table 1] The column header for the feature radius is labeled 'r (kpc)' but the text in Methods says radius is estimated from pixels in the detection map; clarify how the conversion to kpc was made and whether it assumes the Lyα redshift for all features.
  4. [Abstract/Introduction] The phrase 'overwhelming statistical significance' in the abstract should be qualified to refer specifically to the pixel-distribution excess, not to the astrophysical identification, to avoid conflating the two distinct claims.

Circularity Check

0 steps flagged · score 2.0 of 10

No circular reduction of the central claim; only a minor self-citation motivates the fitting function used for the luminosity density.

full rationale

The main detection claim is statistically self-contained: the masked difference-image pixel distribution is fit first by a normal distribution (chi^2 = 562.9 for 129 d.o.f.) and then by the convolution model of Eq. (2) (chi^2 = 139.2 for 126 d.o.f.), and the resulting Delta chi^2 = 423.7 establishes a non-Gaussian positive tail without any fitted parameter being renamed as a prediction. The stacked circumgalactic results are also controlled: on-band minus off-band subtraction with a bogus-redshift null (Fig. 5) means the Ly-alpha, C IV, and Mg II detections do not reduce to their input selection. The only mild self-citation appears in the motivation for the functional form of h(x): 'Motivated by the intensity distribution of the rest-frame ultraviolet continuum of high-redshift galaxies 22 and the H0 column density distribution of QSO absorption lines 23' (Eq. 1); refs 22 and 23 include present authors and adopt the power-law/exponential form as empirical fits, so the derived 'comoving Ly-alpha luminosity density ... 2.9 +/- 2 x 10^40 erg s^-1 Mpc^-3' inherits that self-cited ansatz. This is not load-bearing for the non-Gaussian detection itself, which is independent of the specific fitting form. The paper's real vulnerability is line identification, not circularity: the 422.5 nm filter is degenerate with [O II] at z ~ 0.134, the W_rest > 5 nm cut is computed assuming Ly-alpha and does not exclude high-EW [O II], and the CWI comparison shows 'little correspondence' that the authors 'cannot explain.' The bimodal bootstrap ('we cannot exclude an alternate solution') and the stated need for 'higher-sensitivity observations' are acknowledged fit non-uniqueness, not a reduction of outputs to inputs.

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

The central claims rely on several domain assumptions about the isolation of line emission in the difference image, the Gaussianity of the noise, the ad hoc functional form for the surface brightness distribution, and the cleanliness of the on-band/off-band subtraction. None of these are independently verified within the paper, and the line identification lacks spectroscopic confirmation.

free parameters (5)
  • alpha (power-law index) = 0.66 ± 0.50
    Best-fit index of the truncated power law in Eq. (1), fitted to the masked difference image pixel distribution. It controls the shape of the high-intensity tail and enters the luminosity density estimate.
  • x0 (characteristic intensity) = 1.286 ± 0.035 × 10^-19 erg s^-1 cm^-2 arcsec^-2
    Exponential cutoff scale in Eq. (1), fitted to the pixel distribution. Dominates the first moment.
  • B/A (sky covering ratio) = 0.32 ± 0.20
    Ratio related to the fraction of sky covered by emission above xmin, fitted to the pixel distribution.
  • sigma (noise standard deviation) = 3.3727 ± 0.0021 × 10^-19 erg s^-1 cm^-2 arcsec^-2
    Width of the normal convolution kernel, fitted jointly with the other parameters, though also derivable from the uncertainty image.
  • xbar (background offset) = 5.65 ± 0.14 × 10^-21 erg s^-1 cm^-2 arcsec^-2
    Small mean background term in the convolution, fitted to account for background errors.
assumptions (5)
  • domain assumption The difference image (narrow-band minus luminance) traces line emission at 422.5 nm, with continuum and cirrus subtracted.
    Invoked when forming the difference image and interpreting pixel excesses as Lyα; near bright stars and galaxies the difference may not trace line emission only, as stated in the text.
  • domain assumption Pixel-to-pixel noise in the masked difference image is normally distributed.
    The null hypothesis in Fig. 2 is a normal distribution; modest pixel correlation is corrected by a factor 0.88, but other residual non-Gaussianities could mimic the excess.
  • ad hoc to paper The Lyα surface brightness distribution is a truncated power law with exponential cutoff (Eq. 1).
    Motivated by refs 22 and 23, but the specific functional form is chosen for this analysis and is not derived from theory.
  • domain assumption The on-band minus off-band subtraction removes continuum, dust, and background, leaving only line emission or absorption of the target transition.
    Used in Eq. (12) to interpret the composite images of Fig. 5; assumes foreground and background intensities vary slowly with wavelength and that weighting by redshift uncertainties is correct.
  • domain assumption The dark halo signal in stacked broad-band images is due to dust absorption by the target galaxies.
    Interpretation of the radial profile dip in Fig. 4 assumes a uniform background galaxy density and that the dip is not a stacking artifact or stellar halo. The authors tested several stacking algorithms and Subaru images.

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Pith. "Pith review of Direct Images of the Cosmic Web of Intergalactic and Circumgalactic Gas in the Distant Universe." pith.science (2026). https://pith.science/paper/3V66M2OP

@misc{pith2026241210081,
  author       = {Pith},
  title        = {Pith review of: Direct Images of the Cosmic Web of Intergalactic and Circumgalactic Gas in the Distant Universe},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/3V66M2OP}},
  note         = {Machine review of arXiv:2412.10081}
}
abstract

Most of the baryonic matter of the Universe resides in a highly-ionized gaseous intergalactic medium. This gas flows along dark-matter filaments toward galaxy superclusters, clusters, and groups until it pools around the galaxies into a circumgalactic medium. Eventually, the gas settles into the interstellar medium of the galaxies, where it fuels the successive generations of star formation that ultimately produce the stars and heavy elements that make up galaxies today. The gas has been studied for decades using absorption lines produced by Hydrogen and various ions of heavy elements in the spectra of background quasi-stellar objects (QSOs). But directly imaging the extremely faint glow of this "cosmic web" of intergalactic and circumgalactic gas has remained an elusive goal of observational cosmology. Some recent progress has been made by using imaging spectrographs to record high-redshift Ly$\alpha$ emission, although over only very narrow fields of view. Here we report direct images of intergalactic and circumgalactic gas in the distant Universe obtained using the Condor Array Telescope that we purposely built to reach extremely low-surface-brightness sensitivities over very wide fields of view. We show that these images directly detect and characterize the imprint of Ly$\alpha$ emission from the cosmic web at an overwhelming statistical significance. By stacking portions of the images centered on tens of thousands of galaxies of known redshift, we show that they also reveal extremely faint emission from H$^0$, C$^{3+}$, and Mg$^+$ and absorption from cosmic dust in the tenuous outskirts of the galaxies. Our results demonstrate that sensitive imaging observations can now detect and characterize emission (and absorption) from the cosmic web of intergalactic and circumgalactic gas (and dust).

Figures

Figures reproduced from arXiv: 2412.10081 by the authors.

Figure 5
Figure 5. The narrow-band image is also sensitive to [O II] 372.7 nm emission of redshift [PITH_FULL_IMAGE:figures/full_fig_p004_5.png] view at source ↗

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. The cosmic web's Lyman-$\alpha$ glow at $z \approx 2.5$; hydrodynamic models, dust, and wide-field, narrow-band detection

    astro-ph.CO 2025-10 conditional novelty 6.0 of 10

    Five cosmological simulations predict that the faint ultraviolet excess seen by the Condor telescope at z≈2.5 is Lyman-alpha light from the cosmic web, with measurable detection thresholds for wide-field surveys.

Reference graph

Works this paper leans on

32 extracted references · 9 canonical work pages · cited by 1 Pith paper

  1. [1]

    , Ostriker , J.P

    barticle Cen , R. , Ostriker , J.P. : Where Are the Baryons? II. Feedback Effects . 650 ( 2 ), 560 -- 572 ( 2006 ) 10.1086/506505 https://arxiv.org/abs/astro-ph/0601008 arXiv:astro-ph/0601008 [astro-ph] barticle

    arXiv 2006

  2. [2]

    , Peeples , M.S

    barticle Tumlinson , J. , Peeples , M.S. , Werk , J.K. : The Circumgalactic Medium . 55 ( 1 ), 389 -- 432 ( 2017 ) 10.1146/annurev-astro-091916-055240 https://arxiv.org/abs/1709.09180 arXiv:1709.09180 [astro-ph.GA] barticle

    arXiv 2017

  3. [3]

    , Arrigoni-Battaia , F

    barticle Cantalupo , S. , Arrigoni-Battaia , F. , Prochaska , J.X. , Hennawi , J.F. , Madau , P. : A cosmic web filament revealed in Lyman- emission around a luminous high-redshift quasar . 506 ( 7486 ), 63 -- 66 ( 2014 ) 10.1038/nature12898 https://arxiv.org/abs/1401.4469 arXiv:1401.4469 [astro-ph.CO] barticle

    arXiv 2014

  4. [4]

    , Cantalupo , S

    barticle Gallego , S.G. , Cantalupo , S. , Lilly , S. , Marino , R.A. , Pezzulli , G. , Schaye , J. , Wisotzki , L. , Bacon , R. , Inami , H. , Akhlaghi , M. , Tacchella , S. , Richard , J. , Bouche , N.F. , Steinmetz , M. , Carollo , M. : Stacking the Cosmic Web in fluorescent Ly emission with MUSE . 475 ( 3 ), 3854 -- 3869 ( 2018 ) 10.1093/mnras/sty037 ...

    arXiv 2018

  5. [5]

    The MUSE Extremely Deep Field: the Cosmic Web in Emission at High Redshift

    barticle Bacon , R. , Mary , D. , Garel , T. , Blaizot , J. , Maseda , M. , Schaye , J. , Wisotzki , L. , Conseil , S. , Brinchmann , J. , Leclercq , F. , Abril-Melgarejo , V. , Boogaard , L. , Bouch \'e , N.F. , Contini , T. , Feltre , A. , Guiderdoni , B. , Herenz , C. , Kollatschny , W. , Kusakabe , H. , Matthee , J. , Michel-Dansac , L. , Nanayakkara ...

    work page Pith review arXiv 2021

  6. [6]

    , Darvish , B

    botherref Martin , C. , Darvish , B. , Lin , Z. , Cen , R. , Matuszewski , M. , Morrissey , P. , Neill , J. , Moore , A. : Extensive diffuse lyman-alpha emission correlated with cosmic structure. Nature Astronomy, 1--12 (2023) 10.1038/s41550-023-02054-1 botherref

    doi:10.1038/s41550-023-02054-1 2023

  7. [7]

    Introducing the Condor Array Telescope. 1. Motivation, Configuration, and Performance

    barticle Lanzetta , K.M. , Gromoll , S. , Shara , M.M. , Berg , S. , Valls-Gabaud , D. , Walter , F.M. , Webb , J.K. : Introducing the Condor Array Telescope. I. Motivation, Configuration, and Performance . 135 ( 1043 ), 015002 ( 2023 ) 10.1088/1538-3873/acaee6 https://arxiv.org/abs/2301.06301 arXiv:2301.06301 [astro-ph.IM] barticle

    work page Pith review arXiv 2023

  8. [8]

    , Mackey , M.B

    barticle Hazard , C. , Mackey , M.B. , Shimmins , A.J. : Investigation of the Radio Source 3C 273 By The Method of Lunar Occultations . 197 ( 4872 ), 1037 -- 1039 ( 1963 ) 10.1038/1971037a0 barticle

    doi:10.1038/1971037a0 1963

Show all 32 references
  1. [9]

    : 3C 273 : A Star-Like Object with Large Red-Shift

    barticle Schmidt , M. : 3C 273 : A Star-Like Object with Large Red-Shift . 197 ( 4872 ), 1040 ( 1963 ) 10.1038/1971040a0 barticle

    1963 doi

  2. [10]

    : The Absorption-Line Spectrum of 4c 05.34

    barticle Lynds , R. : The Absorption-Line Spectrum of 4c 05.34 . ApJL 164 , 73 ( 1971 ) 10.1086/180695 barticle

    1971 doi

  3. [11]

    , Spitzer , J

    barticle Bahcall , J.N. , Spitzer , J. Lyman : Absorption Lines Produced by Galactic Halos . 156 , 63 ( 1969 ) 10.1086/180350 barticle

    1969 doi

  4. [12]

    , Young , P.J

    barticle Sargent , W.L.W. , Young , P.J. , Boksenberg , A. , Tytler , D. : The distribution of Lyman-alpha absorption lines in the spectra of six QSOs: evidence for an intergalactic origin. 42 , 41 -- 81 ( 1980 ) 10.1086/190644 barticle

    1980 doi

  5. [13]

    , Crain , R.A

    barticle Schaye , J. , Crain , R.A. , Bower , R.G. , Furlong , M. , Schaller , M. , Theuns , T. , Dalla Vecchia , C. , Frenk , C.S. , McCarthy , I.G. , Helly , J.C. , Jenkins , A. , Rosas-Guevara , Y.M. , White , S.D.M. , Baes , M. , Booth , C.M. , Camps , P. , Navarro , J.F. ...

    2015 arXiv

  6. [14]

    , Puchwein , E

    barticle Bolton , J.S. , Puchwein , E. , Sijacki , D. , Haehnelt , M.G. , Kim , T.-S. , Meiksin , A. , Regan , J.A. , Viel , M. : The Sherwood simulation suite: overview and data comparisons with the Lyman forest at redshifts 2 z 5 . 464 ( 1 ), 897 -- 914 ( 2017 ) 10.1093/mnra...

    2017 arXiv

  7. [15]

    , Weymann , R.J

    barticle Hogan , C.J. , Weymann , R.J. : Lyman-alpha emission from the Lyman-alpha forest . MNRAS 225 , 1 -- 5 ( 1987 ) 10.1093/mnras/225.1.1P barticle

    1987 doi

  8. [16]

    , Porciani , C

    barticle Cantalupo , S. , Porciani , C. , Lilly , S.J. , Miniati , F. : Fluorescent Ly Emission from the High-Redshift Intergalactic Medium . 628 ( 1 ), 61 -- 75 ( 2005 ) 10.1086/430758 https://arxiv.org/abs/astro-ph/0504015 arXiv:astro-ph/0504015 [astro-ph] barticle

    2005 arXiv

  9. [17]

    , Arnouts , S

    barticle Scoville , N. , Arnouts , S. , Aussel , H. , Benson , A. , Bongiorno , A. , Bundy , K. , Calvo , M.A.A. , Capak , P. , Carollo , M. , Civano , F. , Dunlop , J. , Elvis , M. , Faisst , A. , Finoguenov , A. , Fu , H. , Giavalisco , M. , Guo , Q. , Ilbert , O. , Iovino ,...

    2013 arXiv

  10. [18]

    , Lemaux , B.C

    barticle Cucciati , O. , Lemaux , B.C. , Zamorani , G. , Le F \`e vre , O. , Tasca , L.A.M. , Hathi , N.P. , Lee , K.-G. , Bardelli , S. , Cassata , P. , Garilli , B. , Le Brun , V. , Maccagni , D. , Pentericci , L. , Thomas , R. , Vanzella , E. , Zucca , E. , Lubin , L.M. , A...

    2018 arXiv

  11. [19]

    , Gromoll , S

    botherref Lanzetta , K.M. , Gromoll , S. , Shara , M.M. , Berg , S. , Garland , J. , Mancini , E. , Valls-Gabaud , D. , Walter , F.M. , Webb , J.K. : Introducing the Condor Array Telescope. II. Deep imaging observations of the edge-on spiral galaxy NGC 5907 and the NGC 5866 Gr...

    2023

  12. [20]

    : An introduction to matched filters

    barticle Turin , G. : An introduction to matched filters . IRE Transactions on Information Theory 6 ( 3 ), 311 -- 329 ( 1960 ) 10.1109/TIT.1960.1057571 barticle

    1960

  13. [21]

    , Impey , C.D

    barticle Trump , J.R. , Impey , C.D. , Elvis , M. , McCarthy , P.J. , Huchra , J.P. , Brusa , M. , Salvato , M. , Capak , P. , Cappelluti , N. , Civano , F. , Comastri , A. , Gabor , J. , Hao , H. , Hasinger , G. , Jahnke , K. , Kelly , B.C. , Lilly , S.J. , Schinnerer , E. , ...

    2009 arXiv

  14. [22]

    , Yahata , N

    barticle Lanzetta , K.M. , Yahata , N. , Pascarelle , S. , Chen , H.-W. , Fern \'a ndez-Soto , A. : The Star Formation Rate Intensity Distribution Function: Implications for the Cosmic Star Formation Rate History of the Universe . 570 ( 2 ), 492 -- 501 ( 2002 ) 10.1086/339774 ...

    2002 arXiv

  15. [23]

    , Webb , J.K

    barticle Petitjean , P. , Webb , J.K. , Rauch , M. , Carswell , R.F. , Lanzetta , K. : Evidence for structure in the H I column density distribution of QSO absorbers. 262 , 499 -- 505 ( 1993 ) 10.1093/mnras/262.2.499 barticle

    1993 doi

  16. [24]

    , Kajisawa , M

    barticle Taniguchi , Y. , Kajisawa , M. , Kobayashi , M.A.R. , Shioya , Y. , Nagao , T. , Capak , P.L. , Aussel , H. , Ichikawa , A. , Murayama , T. , Scoville , N.Z. , Ilbert , O. , Salvato , M. , Sanders , D.B.B. , Mobasher , B. , Miyazaki , S. , Komiyama , Y. , Le F \`e vre...

    2015 arXiv

  17. [25]

    , Khare , P

    barticle York , D.G. , Khare , P. , Vanden Berk , D. , Kulkarni , V.P. , Crotts , A.P.S. , Lauroesch , J.T. , Richards , G.T. , Schneider , D.P. , Welty , D.E. , Alsayyad , Y. , Kumar , A. , Lundgren , B. , Shanidze , N. , Smith , T. , Vanlandingham , J. , Baugher , B. , Hall ...

    2006

  18. [26]

    , Scranton , R

    barticle M \'e nard , B. , Scranton , R. , Fukugita , M. , Richards , G. : Measuring the galaxy-mass and galaxy-dust correlations through magnification and reddening . 405 ( 2 ), 1025 -- 1039 ( 2010 ) 10.1111/j.1365-2966.2010.16486.x https://arxiv.org/abs/0902.4240 arXiv:0902....

    2010

  19. [27]

    , Groth , E.J

    barticle Peebles , P.J.E. , Groth , E.J. : Statistical analysis of catalogs of extragalactic objects. V. Three-point correlation function for the galaxy distribution in the Zwicky catalog. 196 , 1 -- 11 ( 1975 ) 10.1086/153390 barticle

    1975 doi

  20. [28]

    , Bowen , D.V

    barticle Lanzetta , K.M. , Bowen , D.V. , Tytler , D. , Webb , J.K. : The Gaseous Extent of Galaxies and the Origin of Lyman-Alpha Absorption Systems: A Survey of Galaxies in the Fields of Hubble Space Telescope Spectroscopic Target QSOs . 442 , 538 ( 1995 ) 10.1086/175459 barticle

    1995 doi

  21. [29]

    , Lanzetta , K.M

    barticle Chen , H.-W. , Lanzetta , K.M. , Webb , J.K. : The Origin of C IV Absorption Systems at Redshifts z < 1 : Discovery of Extended C IV Envelopes around Galaxies . 556 ( 1 ), 158 -- 163 ( 2001 ) 10.1086/321537 https://arxiv.org/abs/astro-ph/0104403 arXiv:astro-ph/0104403...

    2001 arXiv

  22. [30]

    , Boiss \'e , P

    barticle Bergeron , J. , Boiss \'e , P. : A sample of galaxies giving rise to Mg II quasar absorption systems. 243 , 344 ( 1991 ) barticle

    1991

  23. [31]

    , Gromoll , S

    botherref Lanzetta , K.M. , Gromoll , S. , Shara , M.M. , Garland , D. James Valls - Gabaud , Walter , F.M. , Webb , J.K. : Introducing the Condor Array Telescope. V. Deep Broad- and Narrow-Band Imaging Observations of the M81 Group . ApJS (2024) botherref

    2024

  24. [32]

    , Ochsenbein , F

    barticle Wenger , M. , Ochsenbein , F. , Egret , D. , Dubois , P. , Bonnarel , F. , Borde , S. , Genova , F. , Jasniewicz , G. , Lalo \"e , S. , Lesteven , S. , Monier , R. : The SIMBAD astronomical database. The CDS reference database for astronomical objects . A&AS 143 , 9 -...

    arXiv

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