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arxiv: 2606.25081 · v1 · pith:6MZVJH72new · submitted 2026-06-23 · 🌌 astro-ph.CO

Cosmology from Clustering of Continuum Galaxies

Jacobo Asorey , Catherine L. Hale , Sebastian von Hausegger , David Parkinson , Chandra Shekhar Saraf , Jonah D. Wagenveld , Benedict Bahr-Kalus , Syed Faisal ur Rahman
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Ziad Sakr
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Pith reviewed 2026-06-25 22:51 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords radio continuum galaxiesangular clusteringSKAO surveycosmologyredshift distributiongalaxy biasmagnification biastelescope systematics
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The pith

A 20,000 square degree SKAO survey reaches microJansky sensitivity and can detect 300-400 million radio continuum galaxies whose angular clustering probes cosmology.

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

Radio continuum galaxies trace the large-scale matter distribution and can inform initial conditions, dark matter, and dark energy. Their use requires models for redshift distribution, galaxy bias, and magnification bias because sources lack easy radial positions and cross-identifications are difficult. The paper examines a specific SKAO survey covering 20,000 square degrees with 10,000 hours of integration in AA4 configuration. This setup reaches O(μJy/beam) depth and yields the largest radio continuum sample to date, exceeding prior SKA Red Book assumptions. Mocks that incorporate telescope systematics are used to forecast the angular clustering signal and to identify needed data corrections.

Core claim

The distribution of radio continuum galaxies is a useful probe of the matter distribution. For the described 20,000 sq. deg. SKAO survey in AA4 configuration with 10,000 hours, O(μJy/beam) sensitivities are reached and O(300-400 million) radio sources are detected. This sample size surpasses the number assumed for the previous SKA cosmology Red Book. Angular clustering is predicted from mocks that include potential telescope systematics, and the paper discusses data corrections required when those systematics cannot be fully modeled.

What carries the argument

Mocks that incorporate potential telescope systematics to forecast the angular clustering of the radio continuum sources.

If this is right

  • The survey yields the largest sample of radio continuum galaxies assembled to date.
  • The sample exceeds the source numbers used in the prior SKA cosmology Red Book.
  • Angular clustering predictions from the mocks indicate which telescope systematics must be corrected to extract cosmology.
  • Reliable cosmological inferences from the clustering require accurate inputs for redshift distribution, galaxy bias, and magnification bias.

Where Pith is reading between the lines

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

  • If the required population models prove accurate, cross-correlations between this radio sample and optical or infrared catalogs could supply the missing radial information.
  • The same mock-based forecasting approach could be repeated for deeper or wider configurations of other radio arrays to test scalability.
  • Deviations between observed and predicted clustering after corrections would point to unmodeled evolution in the radio galaxy population itself.

Load-bearing premise

Accurate measurements or models of the redshift distribution of radio sources, the galaxy bias, and the flux distribution are available so that reliable cosmological inferences can be made from the clustering signal.

What would settle it

A measured source count well below 300 million or an angular clustering amplitude that deviates from the mock predictions after all modeled corrections would show the survey does not deliver the forecasted cosmological information.

Figures

Figures reproduced from arXiv: 2606.25081 by Benedict Bahr-Kalus, Catherine L. Hale, Chandra Shekhar Saraf, David Parkinson, Jacobo Asorey, Jonah D. Wagenveld, Sebastian von Hausegger, Syed Faisal Ur Rahman, Ziad Sakr.

Figure 1
Figure 1. Figure 1: Left: Comparisons of this simulated survey (blue) compared to continuum surveys from SKA precursors of the effective 1.4 GHz rms (assuming 𝑆𝜈 ∝ 𝜈 −0.7 ) and area covered. Points are coloured by their frequency and the marker size indicates the resolution. Right: Expected source numbers with flux density limit in this survey (grey, using simulations outlined in Section 5) to previous/current surveys (dashed… view at source ↗
Figure 2
Figure 2. Figure 2: Estimated rms distribution of a planned 20 000 sq deg, 10 000 h AA4 survey (incl. galaxy). Firstly, we generate a selection of potentially detectable input sources across the potential field of view for such a survey with the SKAO. We sample source positions across the field of view from cosmological matter density fields simulated with GLASS (Tessore et al., 2023), a simulation framework that efficiently … view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of the over-density (𝛿) as in Equation 1 for a 20 000 deg2 survey which includes (left) or excludes (right) the Galactic plane with increasing flux density for no flux cut (top), 20𝜇Jy cut (middle) and 40 𝜇Jy (bottom). Included in the title of each plot is the number of sources expected in the survey. Hale et al., 2025) - thus overcoming the effects of confusion which affects deep surveys such a… view at source ↗
Figure 4
Figure 4. Figure 4: Redshift distribution (𝑁(𝑧)) of the expected radio sources (grey) and split into SFGs (blue) and AGN (red). 6.2 𝐶ℓ predictions for the SKAO In this section we present predictions for the large￾scale structure measurements from the proposed sur￾vey with SKAO AA4 configuration. For that, we have measured the angular power spectra for the dif￾ferent simulated maps described in Section 5. As outlined above, th… view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of the 𝐶ℓ for a variety of flux density (𝑆) and galactic latitude (𝑏) cuts. Solid lines indicate 𝐶ℓ measured from the output catalogue (solid lines) and the dotted lines indicate the 𝐶ℓ measured using weights which account for incompleteness. Shown are: top left: comparison when no galactic cut is applied; top right: when a ±10◦ galactic cut is applied; and bottom: results for flux densities abo… view at source ↗
Figure 6
Figure 6. Figure 6: Relative error on the estimated angular power spectrum for the proposed SKAO AA4 continuum survey and an EMU-like survey. The grey area represents the non-linear scales. Whilst the 1-halo clustering of galaxies (see e.g. Zheng et al., 2005) has been explored thoroughly in the optical and IR (see e.g. Zehavi et al., 2011; Hatfield et al., 2016), this is relatively unexplored in the case of radio continuum s… view at source ↗
read the original abstract

The distribution of radio continuum galaxies is a useful, fast, and accessible probe of the matter distribution in the Universe, enlightening us about the Universe's initial conditions, the physics of dark matter, and the nature of the mysterious dark energy. However, radio continuum galaxies alone cannot easily be localised in the radial direction, and cross-identification of host sources from optical catalogues is challenging across wide area surveys. Moreover, there are several redshift-dependent properties of radio galaxy populations that all need accurate modelling to make reliable inferences about fundamental physics. These include accurate measurements of the redshift distribution of radio sources ($dN/dz$), the coupling between radio galaxies and the underlying matter distribution (quantified by the galaxy bias, $b(z)$), and the true flux distribution $N(S,z)$ of the radio sources (magnification bias). The amount of encoded cosmological information depends on the survey properties and the level of homogeneity across its footprint. In this chapter, we demonstrate the cosmological potential of a 20,000 sq. deg survey with the SKAO in AA4 configuration, using 10,000 hours of observations. Such a survey will reach $\mathcal{O}(\mu\mathrm{Jy/beam)}$ sensitivities and detect $\mathcal{O}$(300-400 million) radio sources, the largest sample of radio continuum galaxies to date. This surpasses the number of sources assumed for the previous SKA cosmology Red Book. We predict the angular clustering of such a survey, using mocks accounting for potential telescope systematics, and discuss which data corrections may be needed when these systematics cannot be accurately modelled.}

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The manuscript forecasts the cosmological potential of angular clustering from radio continuum galaxies in a 20,000 sq. deg. SKAO AA4 survey using 10,000 hours of integration. It claims this survey reaches O(μJy/beam) sensitivity and detects O(300-400 million) sources—exceeding prior SKA Red Book assumptions—and predicts the angular clustering signal via mocks that incorporate telescope systematics while discussing required data corrections. The work emphasizes that reliable cosmological inferences require accurate models of dN/dz, galaxy bias b(z), and magnification bias N(S,z).

Significance. If the input population models prove robust and the mocks accurately capture both systematics and clustering, the result would update expectations for the largest radio-continuum sample available for cosmology, potentially strengthening forecasts for constraints on dark energy and initial conditions beyond previous SKA planning documents. The explicit identification of the three key population parameters as prerequisites for inference is a useful clarification.

major comments (2)
  1. [Abstract] Abstract: the central demonstration consists of predicting angular clustering from mocks that must incorporate dN/dz, b(z) and N(S,z) as inputs, yet no validation, robustness tests against current observational uncertainties, or variation of these inputs is described; because both the quoted source count (300-400 million) and the clustering amplitude derive directly from the same N(S,z) and bias assumptions, any systematic error in those inputs propagates to the claimed cosmological potential and the comparison with the SKA Red Book.
  2. [Abstract] Abstract: the statement that the survey 'surpasses the number of sources assumed for the previous SKA cosmology Red Book' is presented without a quantitative side-by-side comparison of either the predicted clustering amplitude or the resulting cosmological forecast precision, leaving the improvement in cosmological utility unsubstantiated.
minor comments (1)
  1. The manuscript is described as 'this chapter'; the relation to any larger volume or book should be clarified for readers.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive feedback. The comments correctly identify that our forecasts rely on input population models and that the abstract claim of improvement over the SKA Red Book would benefit from more explicit support. We respond to each point below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central demonstration consists of predicting angular clustering from mocks that must incorporate dN/dz, b(z) and N(S,z) as inputs, yet no validation, robustness tests against current observational uncertainties, or variation of these inputs is described; because both the quoted source count (300-400 million) and the clustering amplitude derive directly from the same N(S,z) and bias assumptions, any systematic error in those inputs propagates to the claimed cosmological potential and the comparison with the SKA Red Book.

    Authors: We agree that the forecasts are tied to the chosen fiducial models for dN/dz, b(z) and N(S,z). The manuscript adopts standard literature values for these quantities to generate the mocks and explicitly states in the introduction that accurate modeling of all three is required for reliable cosmological inference. No robustness tests or parameter variations are performed in the current work, as the emphasis is on survey geometry, depth, and telescope systematics rather than population-model uncertainty. We will revise the abstract and discussion to qualify the results as forecasts under current best-estimate inputs, noting that systematic errors in these inputs would propagate to the quoted source counts and clustering amplitude. This clarification will be added without changing the core analysis. revision: partial

  2. Referee: [Abstract] Abstract: the statement that the survey 'surpasses the number of sources assumed for the previous SKA cosmology Red Book' is presented without a quantitative side-by-side comparison of either the predicted clustering amplitude or the resulting cosmological forecast precision, leaving the improvement in cosmological utility unsubstantiated.

    Authors: We accept that the claim would be stronger with a direct comparison. The Red Book used earlier sensitivity assumptions that yielded fewer sources than the updated AA4 configuration and 10,000-hour integration considered here. We will insert a brief quantitative comparison (source numbers and, where straightforward, a note on clustering amplitude scaling) in the revised abstract or main text. A full side-by-side cosmological-parameter forecast is outside the present scope but can be flagged as desirable future work. revision: yes

Circularity Check

0 steps flagged

No significant circularity; forward modeling from standard inputs

full rationale

The paper forecasts source counts and angular clustering for a future SKAO survey by constructing mocks that incorporate external models for dN/dz, b(z) and N(S,z). This is standard forward modeling rather than fitting any parameter to the clustering signal being predicted and then re-presenting the fit as a prediction. No equations or steps in the abstract reduce the output to the inputs by construction, no self-citation chain is load-bearing, and no uniqueness theorem is invoked. The derivation remains independent of the target result and is therefore self-contained.

Axiom & Free-Parameter Ledger

3 free parameters · 1 axioms · 0 invented entities

Only abstract available; ledger reflects the modeling requirements explicitly named as necessary for the central claim.

free parameters (3)
  • redshift distribution dN/dz
    Stated as required for reliable inferences but no specific functional form or fitting procedure given.
  • galaxy bias b(z)
    Stated as required for reliable inferences but no specific functional form or fitting procedure given.
  • magnification bias N(S,z)
    Stated as required for reliable inferences but no specific functional form or fitting procedure given.
axioms (1)
  • domain assumption Radio continuum galaxies trace the underlying matter distribution sufficiently well for clustering to encode cosmological information.
    Abstract opens by calling the distribution 'a useful, fast, and accessible probe of the matter distribution'.

pith-pipeline@v0.9.1-grok · 5845 in / 1433 out tokens · 27740 ms · 2026-06-25T22:51:11.701920+00:00 · methodology

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Reference graph

Works this paper leans on

210 extracted references · 156 canonical work pages · 30 internal anchors

  1. [1]

    2026 ,publisher =

    Jacobo Asorey&Hale and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  2. [2]

    2026 ,publisher =

    Daniele Bertacca and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  3. [3]

    2026 ,publisher =

    Isabella Prandoni and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  4. [4]

    2026 ,publisher =

    Ian Harrison and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  5. [5]

    2026 ,publisher =

    Suman Chatterjee and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  6. [6]

    2026 ,publisher =

    Jacobo Asorey&C.Hale, and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  7. [7]

    Cosmic Dipole Measurements

    Sebastian Von Hausegger and others. Cosmic Dipole Measurements. 2025

    2025

  8. [8]

    CMB Synergies for Cosmology

    Jens Chluba and others. CMB Synergies for Cosmology. 2025

    2025

  9. [9]

    Cosmology from Clustering of Continuum Galaxies

    Jacobo Asorey and Catherine Hale and others. Cosmology from Clustering of Continuum Galaxies. 2025

    2025

  10. [10]

    Enhancing Continuum Galaxy Surveys with VLBI

    David Parkinson and others. Enhancing Continuum Galaxy Surveys with VLBI. 2025

    2025

  11. [11]

    Galaxy Clusters Viewed with Strong and Weak Lensing

    Mamta Pommier and others. Galaxy Clusters Viewed with Strong and Weak Lensing. 2025

    2025

  12. [12]

    Weak Lensing with SKAO: Cosmic Shear Cosmology

    Ian Harrison and others. Weak Lensing with SKAO: Cosmic Shear Cosmology. 2025

    2025

  13. [13]

    Weak Lensing II (Shape Measurement)

    Priyamvad Tripathi and others. Weak Lensing II (Shape Measurement). 2025

    2025

  14. [14]

    Cosmology from Nx2pt Combinations

    Ian Harrison and others. Cosmology from Nx2pt Combinations. 2025

    2025

  15. [15]

    Cosmology with 21cm Intensity Mapping

    Laura Wolz and others. Cosmology with 21cm Intensity Mapping. 2025

    2025

  16. [16]

    Observational frontiers in 21cm Intensity Mapping: lesson learned from precursors

    Jingying Wang and others. Observational frontiers in 21cm Intensity Mapping: lesson learned from precursors. 2025

    2025

  17. [17]

    Observational frontiers in 21cm Intensity Mapping: lesson learned from pathfinders

    Yichao Li and others. Observational frontiers in 21cm Intensity Mapping: lesson learned from pathfinders. 2025

    2025

  18. [18]

    Methodological frontiers in 21cm Intensity Mapping: the treatment of systematics and foreground contanimation

    Marta Spinelli and others. Methodological frontiers in 21cm Intensity Mapping: the treatment of systematics and foreground contanimation. 2025

    2025

  19. [19]

    Methodological frontiers in 21cm Intensity Mapping: beyond power spectrum solution for the interpretation of the cosmological signalar Cosmology

    Suman Majumdar and others. Methodological frontiers in 21cm Intensity Mapping: beyond power spectrum solution for the interpretation of the cosmological signalar Cosmology. 2025

    2025

  20. [20]

    21cm Intensity Mapping on Small Scales

    Laura Wolz and others. 21cm Intensity Mapping on Small Scales. 2025

    2025

  21. [21]

    Simulations of Cosmological HI Signals

    Tommaso Ronconi and others. Simulations of Cosmological HI Signals. 2025

    2025

  22. [22]

    Tully-Fisher Cosmology with HI Galaxies

    Joel Mayor and others. Tully-Fisher Cosmology with HI Galaxies. 2025

    2025

  23. [23]

    BAO and RSD Cosmolgy with HI Galaxies

    Phil Bull and others. BAO and RSD Cosmolgy with HI Galaxies. 2025

    2025

  24. [24]

    Beyond LCDM I (tests of General Relativity)

    Stefano Camera and others. Beyond LCDM I (tests of General Relativity). 2025

    2025

  25. [25]

    Beyond LCDM II (tests of Inflation)

    Jose Fonseca and others. Beyond LCDM II (tests of Inflation). 2025

    2025

  26. [26]

    Gravitational Wave Synergies for Cosmology

    Marta Spinelli and others. Gravitational Wave Synergies for Cosmology. 2025

    2025

  27. [27]

    FRB Synergies for Cosmology

    Robert Reischke and others. FRB Synergies for Cosmology. 2025

    2025

  28. [28]

    Synergies between Line Intensity Mapping Experiments

    Suman Majumdar and others. Synergies between Line Intensity Mapping Experiments. 2025

    2025

  29. [29]

    Constraints on Particle Dark Matter

    Marco Regis and others. Constraints on Particle Dark Matter. 2025

    2025

  30. [30]

    Fast Simultaneous Surveys with On-the-Fly Mapping

    Suman Chatterjee and others. Fast Simultaneous Surveys with On-the-Fly Mapping. 2025

    2025

  31. [32]

    2015 , publisher=

    Advancing Astrophysics with the Square Kilometre Array (AASKA14) , author=. 2015 , publisher=

    2015

  32. [33]

    Mo, H. J. and White, Simon D. M. , title =. , volume =. 1996 , eprint =

    1996

  33. [34]

    Wilman, R. J. and Miller, L. and Jarvis, M. J. and Mauch, T. and Levrier, F. B. and Abdalla, F. B. and Rawlings, S. and Klöckner, H.-R. and Obreschkow, D. and Olteanu, D. and Young, S. , title =. , volume =. 2008 , eprint =

    2008

  34. [35]

    Probing primordial non-Gaussianity via iSW measurements with SKA continuum surveys , journal =

    Alvise Raccanelli and Olivier Dor. Probing primordial non-Gaussianity via iSW measurements with SKA continuum surveys , journal =. 2015 , volume =. 1406.0010 , archivePrefix=

    Pith/arXiv arXiv 2015

  35. [36]

    Ferreira and Julian Borrill , title =

    Chris Blake and Pedro G. Ferreira and Julian Borrill , title =. , volume =. 2004 , eprint =

    2004

  36. [43]

    Sheth and H

    Ravi K. Sheth and H. J. Mo and Giuseppe Tormen , title =. , volume =. 2001 , eprint =

    2001

  37. [44]

    Abdalla , title =

    Anais Rassat and Kate Land and Ofer Lahav and Filipe B. Abdalla , title =. , volume =. 2007 , eprint =

    2007

  38. [46]

    and Santos, Mario G

    Ferramacho, Luis D. and Santos, Mario G. and Jarvis, Matt J. and Camera, Stefano , title =. , volume =. 2014 , eprint =

    2014

  39. [48]

    and Sherwin, Blake D

    Allison, Rupert and Lindsay, Sam N. and Sherwin, Blake D. and de Bernardis, Francesco and Bond, J. Richard and Calabrese, Erminia and Devlin, Mark J. and Dunkley, Joanna and Gallardo, Patrick and Henderson, Shawn and Hincks, Adam D. and Hlozek, Renee and Jarvis, Matt and Kosowsky, Arthur and Louis, Thibaut and Madhavacheril, Mathew and McMahon, Jeff and M...

    2015

  40. [49]

    Canadian Journal of Physics , year =

    Syed Faisal ur Rahman , title =. Canadian Journal of Physics , year =. doi:10.1139/cjp-2014-0339 , eprint =

    work page doi:10.1139/cjp-2014-0339 2014

  41. [50]

    Lensing corrections to features in the angular two-point correlation function and power spectrum , author =. Phys. Rev. D , volume =. 2008 , month =

    2008

  42. [53]

    Unified Schemes for Radio-Loud Active Galactic Nuclei

    Unified Schemes for Radio-Loud Active Galactic Nuclei. , keywords =. doi:10.1086/133630 , archivePrefix =. astro-ph/9506063 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/133630

  43. [59]

    , keywords =

    The many lives of active galactic nuclei: cooling flows, black holes and the luminosities and colours of galaxies. , keywords =. doi:10.1111/j.1365-2966.2005.09675.x , archivePrefix =. astro-ph/0508046 , primaryClass =

    work page doi:10.1111/j.1365-2966.2005.09675.x 2005

  44. [60]

    Observational Evidence of AGN Feedback

    Observational Evidence of Active Galactic Nuclei Feedback. , keywords =. doi:10.1146/annurev-astro-081811-125521 , archivePrefix =. 1204.4114 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081811-125521

  45. [61]

    Calibrating Extinction-Free Star Formation Rate Diagnostics with 33GHz Free-Free Emission in NGC6946

    Calibrating Extinction-free Star Formation Rate Diagnostics with 33 GHz Free-free Emission in NGC 6946. , keywords =. doi:10.1088/0004-637X/737/2/67 , archivePrefix =. 1105.4877 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/737/2/67

  46. [64]

    The Astronomical Journal , volume=

    The NRAO VLA sky survey , author=. The Astronomical Journal , volume=. 1998 , publisher=

    1998

  47. [65]

    The LOFAR Two-metre Sky Survey. I. Survey description and preliminary data release. , keywords =. doi:10.1051/0004-6361/201629313 , archivePrefix =. 1611.02700 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629313

  48. [68]

    EMU: Evolutionary Map of the Universe

    EMU: Evolutionary Map of the Universe. , keywords =. doi:10.1071/AS11021 , archivePrefix =. 1106.3219 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1071/as11021

  49. [71]

    Probing the Radio Loud/Quiet AGN dichotomy with quasar clustering

    Probing the radio loud/quiet AGN dichotomy with quasar clustering. , keywords =. doi:10.1051/0004-6361/201526433 , archivePrefix =. 1611.08630 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201526433

  50. [72]

    A new analysis of low-frequency radio luminosity as a star-formation tracer in the Lockman Hole region

    The LOFAR Two-metre Sky Survey Deep Fields. A new analysis of low-frequency radio luminosity as a star-formation tracer in the Lockman Hole region. , keywords =. doi:10.1051/0004-6361/202141286 , archivePrefix =. 2109.06735 , primaryClass =

    work page doi:10.1051/0004-6361/202141286

  51. [73]

    A new model for NVSS galaxy catalogue using the redshift distribution and halo minimum mass

    A new model for NVSS galaxy catalogue using the redshift distribution and halo minimum mass. arXiv e-prints , keywords =. doi:10.48550/arXiv.1312.0530 , archivePrefix =. 1312.0530 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1312.0530

  52. [74]

    The clustering of radio galaxies: biasing and evolution versus stellar mass

    The Clustering of Radio Galaxies: Biasing and Evolution versus Stellar Mass. , keywords =. doi:10.1088/0004-637X/812/1/85 , archivePrefix =. 1505.06817 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/812/1/85

  53. [75]

    The angular two-point correlation of NVSS galaxies revisited

    Angular two-point correlation of NVSS galaxies revisited. , keywords =. doi:10.1051/0004-6361/201526956 , archivePrefix =. 1507.02160 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201526956

  54. [76]

    , keywords =

    CENSORS: A Combined EIS-NVSS Survey Of Radio Sources - I. Sample definition, radio data and optical identifications. , keywords =. doi:10.1046/j.1365-2966.2003.07125.x , archivePrefix =. astro-ph/0308401 , primaryClass =

    work page doi:10.1046/j.1365-2966.2003.07125.x 2003

  55. [77]

    , keywords =

    CENSORS: A Combined EIS-NVSS Survey of Radio Sources - II. Infrared imaging and the K-z relation. , keywords =. doi:10.1111/j.1365-2966.2005.09916.x , archivePrefix =. astro-ph/0603655 , primaryClass =

    work page doi:10.1111/j.1365-2966.2005.09916.x 2005

  56. [78]

    Thermal disc emission from a rotating black hole: X-ray polarization signatures.Mon

    A Combined EIS-NVSS Survey Of Radio Sources (CENSORS) - III. Spectroscopic observations. , keywords =. doi:10.1111/j.1365-2966.2008.12786.x , archivePrefix =. 0802.1158 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.12786.x 2008

  57. [79]

    , keywords =

    The LBDS Hercules sample of mJy radio sources at 1.4 GHz - II. Redshift distribution, radio luminosity function, and the high-redshift cut-off. , keywords =. doi:10.1046/j.1365-8711.2001.04934.x , archivePrefix =. astro-ph/0107048 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.04934.x 2001

  58. [80]

    The LOFAR Two-metre Sky Survey. III. First data release: Optical/infrared identifications and value-added catalogue. , keywords =. doi:10.1051/0004-6361/201833564 , archivePrefix =. 1811.07927 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833564

  59. [81]

    The LOFAR Two-metre Sky Survey. IV. First Data Release: Photometric redshifts and rest-frame magnitudes. , keywords =. doi:10.1051/0004-6361/201833562 , archivePrefix =. 1811.07928 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833562

  60. [83]

    , keywords =

    Cosmology from LOFAR Two-metre Sky Survey Data Release 2: Cross-correlation with the cosmic microwave background. , keywords =. doi:10.1051/0004-6361/202347728 , archivePrefix =. 2412.14825 , primaryClass =

    work page doi:10.1051/0004-6361/202347728

  61. [87]

    , keywords =

    Photometric Redshifts and Stellar Masses for Galaxies from the DESI Legacy Imaging Surveys. , keywords =. doi:10.3847/1538-4365/ab1847 , adsurl =

    work page doi:10.3847/1538-4365/ab1847

  62. [88]

    The VLA-COSMOS 3 GHz Large Project: The cosmic star formation history since z~5

    The VLA-COSMOS 3 GHz Large Project: Cosmic star formation history since z 5. , keywords =. doi:10.1051/0004-6361/201629436 , archivePrefix =. 1703.09724 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629436

  63. [89]

    The VLA-COSMOS 3~GHz Large Project: Cosmic evolution of radio AGN and implications for radio-mode feedback since z~5

    The VLA-COSMOS 3 GHz Large Project: Cosmic evolution of radio AGN and implications for radio-mode feedback since z 5. , keywords =. doi:10.1051/0004-6361/201730685 , archivePrefix =. 1705.07090 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201730685

  64. [90]

    , keywords =

    MIGHTEE: Multi-wavelength counterparts in the COSMOS field. , keywords =. doi:10.1093/mnras/stad3307 , archivePrefix =. 2310.17409 , primaryClass =

    work page doi:10.1093/mnras/stad3307

  65. [91]

    arXiv e-prints , keywords =

    EMU: Cross-correlating EMU Pilot Survey 1 with Dark Energy Survey to constrain the radio galaxy redshift distribution. arXiv e-prints , keywords =. doi:10.48550/arXiv.2505.05821 , archivePrefix =. 2505.05821 , primaryClass =

    work page internal anchor Pith review doi:10.48550/arxiv.2505.05821

  66. [92]

    , keywords =

    Cross-correlating radio continuum surveys and CMB lensing: constraining redshift distributions, galaxy bias, and cosmology. , keywords =. doi:10.1093/mnras/stab046 , archivePrefix =. 2009.01817 , primaryClass =

    work page doi:10.1093/mnras/stab046 2009

  67. [95]

    The large-scale structure of the universe

  68. [102]

    The Origin of Radio Emission from Radio-Quiet AGN

    The origin of radio emission from radio-quiet active galactic nuclei. Nature Astronomy , keywords =. doi:10.1038/s41550-019-0765-4 , archivePrefix =. 1902.05917 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-019-0765-4 1902

  69. [103]

    , keywords =

    MIGHTEE: A first look at MIGHTEE quasars. , keywords =. doi:10.1093/mnras/staf1187 , archivePrefix =. 2507.12046 , primaryClass =

    work page doi:10.1093/mnras/staf1187

  70. [107]

    , keywords =

    MIGHTEE: the nature of the radio-loud AGN population. , keywords =. doi:10.1093/mnras/stac2140 , archivePrefix =. 2207.12379 , primaryClass =

    work page doi:10.1093/mnras/stac2140

  71. [108]

    The star-formation rate-radio luminosity relation at low frequencies

    The LOFAR Two-metre Sky Survey Deep Fields. The star-formation rate-radio luminosity relation at low frequencies. , keywords =. doi:10.1051/0004-6361/202039343 , archivePrefix =. 2011.08196 , primaryClass =

    work page doi:10.1051/0004-6361/202039343 2011

  72. [110]

    , keywords =

    The radio emission from active galactic nuclei. , keywords =. doi:10.1051/0004-6361/202140791 , archivePrefix =. 2104.04519 , primaryClass =

    work page doi:10.1051/0004-6361/202140791

  73. [111]

    The ELAIS-N1 field

    The LOFAR Two-metre Sky Survey: Deep Fields Data Release 2: I. The ELAIS-N1 field. , keywords =. doi:10.1051/0004-6361/202452930 , archivePrefix =. 2501.04093 , primaryClass =

    work page doi:10.1051/0004-6361/202452930

  74. [112]

    The LOFAR Two-meter Sky Survey: Deep Fields Data Release 1. I. Direction-dependent calibration and imaging. , keywords =. doi:10.1051/0004-6361/202038804 , archivePrefix =. 2011.08328 , primaryClass =

    work page doi:10.1051/0004-6361/202038804 2011

  75. [113]

    , keywords =

    GaLactic and Extragalactic All-sky Murchison Widefield Array eXtended (GLEAM-X) survey II: Second Data Release. , keywords =. doi:10.1017/pasa.2024.57 , archivePrefix =. 2406.06921 , primaryClass =

    work page doi:10.1017/pasa.2024.57 2024

  76. [115]

    RAS Techniques and Instruments , year = 2024, month = jan, volume =

    ContinUNet: fast deep radio image segmentation in the Square Kilometre Array era with U-Net. RAS Techniques and Instruments , year = 2024, month = jan, volume =. doi:10.1093/rasti/rzae019 , adsurl =

    work page doi:10.1093/rasti/rzae019 2024

  77. [116]

    PyBDSF: Python Blob Detection and Source Finder

  78. [117]

    DeepSource: Point Source Detection using Deep Learning

    DEEPSOURCE: point source detection using deep learning. , keywords =. doi:10.1093/mnras/stz131 , archivePrefix =. 1807.02701 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz131

  79. [119]

    Source-finding for the Australian Square Kilometre Array Pathfinder

    Source-Finding for the Australian Square Kilometre Array Pathfinder. , keywords =. doi:10.1071/AS12028 , archivePrefix =. 1208.2479 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1071/as12028

  80. [126]

    Theoretical Models of the Halo Occupation Distribution: Separating Central and Satellite Galaxies

    Theoretical Models of the Halo Occupation Distribution: Separating Central and Satellite Galaxies. , keywords =. doi:10.1086/466510 , archivePrefix =. astro-ph/0408564 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/466510

Showing first 80 references.