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The Radio Spectral Energy Distribution and Star Formation Calibration in MIGHTEE-COSMOS Highly Star-Forming Galaxies at 1.5 < z < 3.5

T0 review · 4 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read The paper claims that radio SED shapes evolve with star formation in 160 starbursts at $1.5<z<3.5$, and that using a variable synchrotron spectral index makes the infrared-radio correlation and MRC-based SFR calibrations redshift-invariant.

desk verdict The MRC luminosities and SFR calibrations are genuinely useful, but the B–(1+z) dynamo claim is largely a repackaged luminosity–redshift scaling and should be reframed before publication. read the letter →

arxiv 2506.16275 v1 pith:EU22GN2X submitted 2025-06-19 astro-ph.GA

Fatemeh Tabatabaei , Maryam Khademi , Matt J. Jarvis , Russ Taylor , Imogen H. Whittam , Fangxia An , Reihaneh Javadi , Eric J. Murphy
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Mattia Vaccari
This is my paper · ORCID
classification astro-ph.GA
keywords radiospectralenergydistributionstarformationratecalibrationinfrared-radiocorrelationsynchrotronindexmagneticfieldMIGHTEE-COSMOSstarburstgalaxieshigh-redshift
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

By fitting rest-frame radio spectral energy distributions of 160 highly star-forming galaxies at $1.5

What carries the argument

The load-bearing object is the rest-frame radio SED fit, modeled as a thermal free-free component with spectral index $0.1$ plus a nonthermal synchrotron power law with fitted index $\alpha_{\rm nt}$, using Bayesian MCMC on MeerKAT 1.3 GHz, VLA 1.4/3 GHz, and GMRT 0.325/0.61 GHz fluxes. The fitted $\alpha_{\rm nt}$ is then inserted in the k-correction to build monochromatic and integrated 1-10 GHz luminosities, to estimate the equipartition field through the luminosity and stellar-mass scaling $B=B_0(L_{\rm nt}/L_{\rm nt,0})^{1/4}(M_\star/M_{\star,0})^{-0.1}$, and to recalculate the $q$-parameter and SFR calibrations. The mechanism that carries the main claim is simple: replacing a fixed spectral index with the measured, redshift-dependent index changes the k-correction enough to remove the apparent infrared-radio correlation evolution.

What would settle it

Measure magnetic fields in $1.5<z<3.5$ starbursts with a method that does not assume equipartition, such as Faraday rotation measures of background polarized sources; if the field does not rise as $(1+z)^{0.7}$, the dynamo claim fails. Alternatively, fit radio SEDs for a sample that includes both $z\simeq1.5$ and $z\simeq3.5$ starbursts matched in specific star formation rate: the paper's interpretation predicts no residual $\alpha_{\rm nt}$-redshift trend once sSFR is fixed.

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Extended reading notes

Core claim

On its own terms, the central discovery is that the radio SED of distant starbursts is not a fixed power law. Bayesian fits of $S_{\nu_e}=A_{\rm th}\nu_e^{-0.1}+A_{\rm nt}\nu_e^{-\alpha_{\rm nt}}$ to MeerKAT, VLA, and GMRT photometry give a mean $\alpha_{\rm nt}=0.75$, flatter than local star-forming galaxies, and the index flattens with redshift and with sSFR. Because the partial correlation of $\alpha_{\rm nt}$ with redshift at fixed sSFR is weak, the redshift trend is attributed to the cosmic evolution of star formation activity. With this variable index in the k-correction, the infrared-radio correlation parameter is $q=2.2$ with no redshift or stellar-mass dependence over $1.5<z<3.5$, while a fixed $\alpha_{\rm nt}=0.75$ would instead produce an artificial decline roughly as $(1+z)^{-0.16}$. Applying the same variable-SED treatment, the integrated 1-10 GHz MRC luminosity calibrates SFR through ${\rm SFR}\propto{\rm MRC}^{0.83}$ with no residual redshift trend and tighter scatter than monochromatic luminosities. The equipartition magnetic field increases as $B\propto(1+z)^{0.7}$ and $B\propto{\rm SFR}^{0.25\pm0.05}$, which the paper interprets as a small-scale turbulent dynamo operating in high-redshift starbursts.

Load-bearing premise

The magnetic-field and dynamo conclusions assume that cosmic-ray energy and magnetic energy are in equipartition and that the nearby starburst NGC 253 is a fair reference, and because the field is derived from the same synchrotron luminosity whose redshift growth is fitted, that assumption carries the claimed $B\propto(1+z)^{0.7}$ result.

Editorial extensions

If this is right

  • Using a single fixed spectral index in k-corrections over $1.5<z<3.5$ introduces an artificial redshift trend in $q$ of roughly $(1+z)^{-0.16}$, so previously reported IRRC evolution should be re-examined with variable SED shapes.
  • The integrated MRC luminosity, recoverable from 1.3 and 3 GHz luminosities via ${\rm MRC}=-0.62\,\nu L_{1.3}+2.89\,\nu L_3$, is a tighter and redshift-invariant SFR tracer than monochromatic luminosities.
  • The local MRC-based SFR calibration, ${\rm SFR}_{\rm MRC}\propto{\rm MRC}^{0.8}$, remains applicable at high redshift, with near-linear agreement with TIR-based SFR at $b=1.00\pm0.04$.
  • The B-SFR slope of roughly $0.25$ to $0.3$ supports a small-scale turbulent dynamo as the dominant magnetic-field amplification mechanism in high-redshift starbursts.
  • Because the radio luminosity is super-linearly enhanced relative to the infrared luminosity, the IRRC deviates from linearity and $q$ is lower at $1.5<z<3.5$ than in the local universe.

Reading between the lines

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

  • A reader-level extension: the claimed $B\propto(1+z)^{0.7}$ is not fully independent, because the equipartition formula derives the field from the same synchrotron luminosity whose redshift evolution is fitted; independent magnetic probes are needed to confirm the dynamo interpretation.
  • A testable extension of the paper's logic: apparent stellar-mass trends in the IRRC reported at lower redshifts should also flatten once the radio SED shape is fitted, rather than a fixed spectral index being assumed.
  • A further extension: if flat synchrotron spectra and strong turbulent fields are common in high-redshift starbursts, cosmic-ray pressure gradients may contribute to driving galactic outflows, a consequence that could be tested with radio halo morphology and outflow kinematics.
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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

4 major / 5 minor

Summary. The paper uses MeerKAT, VLA, and GMRT continuum measurements to construct rest-frame radio SEDs for 160 star-forming galaxies at 1.5 < z < 3.5 in the MIGHTEE-COSMOS field. A Bayesian MCMC fit separates (in principle) thermal free-free and nonthermal synchrotron components, from which the authors derive the mid-radio continuum (MRC) luminosity, equipartition magnetic field strengths, an evolving nonthermal spectral index, redshift-invariant infrared-radio correlation parameters, and SFR calibrations. The central claims are that the synchrotron spectral index flattens with redshift and sSFR, that B evolves as (1+z)^0.7 and as SFR^0.3 via a small-scale dynamo, and that the IRRC is redshift-invariant once SED evolution is included.

Significance. If the claims hold, this is a valuable step: it is one of the first attempts to go beyond a fixed radio spectral index at high redshift, it produces a high-z MRC luminosity and SFR calibration, and it offers a concrete explanation for the previously reported redshift evolution of the IRRC. The paper is honest in presenting sample-selection tests in Appendix C and in providing detailed tables of the fitted SED parameters and luminosities. However, the magnetic-field and dynamo conclusions are not independent measurements: they are largely algebraic consequences of the equipartition conversion applied to the fitted luminosity-redshift relation. The SED-evolution and IRRC claims also rest on a small number of detected thermal components and on SED fits to only five low-SNR points, so the significance of the physical interpretation is currently limited.

major comments (4)
  1. [§3.1, §6.1; Eq. (12)] Only 11 of the 160 galaxies have a detected thermal component, and for the remaining 149 galaxies the fitted αnt is the power-law index of the total synchrotron-plus-free-free emission rather than a pure nonthermal index. Because any undetected free-free component makes the total spectrum flatter than the true αnt, the reported mean αnt = 0.75 and the flattening with redshift in Eq. (12) and with sSFR in Eq. (13) cannot be interpreted as evidence for more energetic cosmic-ray electrons unless the thermal fraction is shown to be negligible on a per-galaxy basis. The Hα cross-check in Appendix B covers only six galaxies, most of them lower limits, and is insufficient to validate this assumption.
  2. [§5 Eq. (11), §6.2 Eqs. (15)-(16), Appendix C Eq. (C1)] The B–(1+z)^0.7 and B–SFR^0.3 results are essentially algebraic consequences of Eq. (11) applied to the fitted luminosity–redshift relation. Equation (11) gives B ∝ Lnt^1/4, and Appendix C Eq. (C1) fits log10(νL1.3) = (2.9±0.2) log10(1+z) + const for the same galaxies; with the sample synchrotron-dominated this yields B ∝ (1+z)^0.72, matching Eq. (15). Similarly, combining Eq. (11) with the SFR–MRC relation Eq. (21), whose slope is 0.83, gives B ∝ SFR^0.30 by construction. These relations therefore do not constitute an independent test of the small-scale dynamo; the authors should state this degeneracy explicitly and either present the full equipartition calculation including the αnt dependence of Eq. (D5) or add a test that removes the Lnt–z and Lnt–SFR scalings before interpreting the residuals.
  3. [§6.3, Eq. (17), Fig. 9] The claim that the IRRC is redshift-invariant when SED evolution is included rests on using the per-galaxy αnt, which is itself fitted from the same noisy five-point SEDs, to compute L1.3. If the fitted αnt–z relation in Eq. (12) is partly an artifact of the single power-law fitting or of the exclusion of curved SEDs (Section 3.1), the k-correction can spuriously remove a real q–z trend. The q_MRC version in Fig. 9c is less affected by k-correction and is a better test; the authors should make it the primary evidence and also report the fit to q_MRC with and without the small fraction of galaxies with detected thermal emission.
  4. [§3.1, Appendix C] The final sample excludes galaxies whose residuals exceed 50% at 0.3 and 0.6 GHz because a curved SED fits those sources better. Appendix C tests the SNR>1 selection and flux-density cuts, but it does not test the effect of this explicit curvature-based exclusion. If low-frequency curvature is more common at higher redshift or higher sSFR, the selection could produce the observed αnt flattening in Eqs. (12) and (13) and, through Eq. (11), part of the B–z trend. An analysis including the excluded sources with a curved model, or at least a sensitivity test on the full 189-galaxy sample, is needed.
minor comments (5)
  1. [§5] The assumed random-inclination average ⟨(cos i/cos i0)^{-1/4}⟩ is not approximately 1 for an isotropic distribution; with i0 = 78° it evaluates to about 0.90, shifting the B normalization by roughly 10%. The authors should quantify this rather than stating it is ≃1.
  2. [Abstract, §6.2, §7] The abstract and summary state B ∝ SFR^0.3, but Eq. (16) gives B = 10^1.5 SFR^(0.25±0.05); the text should match the fitted exponent or explain why the rounded value is preferred.
  3. [§4, Eq. (10)] The MRC calibration coefficients a and b are reported without uncertainties; given that a = -0.62 and b = 2.89 are likely strongly covariant, the authors should provide the covariance and validate the relation with a hold-out sample or bootstrap.
  4. [§6.3] The value q = 2.2 ± 0.01 is the standard error of the mean, while the scatter about the mean is 0.2 dex; the paper should report the dispersion as the primary uncertainty when comparing with other samples.
  5. [Fig. 11] The legend in the left and middle panels labels the upper redshift bin as 2 < z < 4.5, whereas the text and sample selection use 2 < z < 3.5; this should be corrected.

Circularity Check

1 steps flagged · score 6.0 of 10

The B–(1+z)^0.7 result is the fitted Lnt–z slope raised to the 1/4 power by Eq. (D7), so the dynamo conclusion is not independently tested.

  1. fitted input called prediction [Appendix D Eq. (D7); Appendix C Eq. (C1); Section 6.2 Eq. (15)]
    "B = B0 (cos(i)/cos(i0))^{-1/4} (Lnt/Lnt0)^{1/4} (M*/M*0)^{-0.1}, ... log10(νL1.3) = (2.9 ± 0.2) log10(1+z) + (38.81 ± 0.12), ... B/µG = (55 ± 7) × (1+z)^{0.7±0.1}"

    Eq. (D7) defines B as a fixed 1/4-power of the synchrotron luminosity Lnt. Appendix C fits the same sample's log10(νL1.3) against log10(1+z), obtaining a slope of 2.9. Because the sample is synchrotron-dominated, Lnt essentially follows this fitted luminosity–redshift relation, so B ∝ Lnt^{1/4} ∝ (1+z)^{2.9/4} ≈ (1+z)^{0.725}. The reported B ∝ (1+z)^{0.7±0.1} in Eq. (15) is therefore algebraically imported from the fitted Lnt–z relation rather than being an independent measurement of field amplification. The full equipartition formula Eq. (D5) contains an αnt-dependent prefactor that Eq. (D7) omits; since αnt itself flattens with redshift in Eq. (12), the omitted spectral-index term can also contribute to the apparent B–z trend.

full rationale

The SED modeling, MRC luminosity integration, and the αnt–sSFR correlation are self-contained empirical results, and the IRRC invariance is presented as a differential test against a fixed spectral index, which is legitimate modeling rather than a purely formal equivalence. However, the headline magnetic-field evolution claim reduces by construction: Eq. (D7) makes B a one-quarter power of Lnt, and Appendix C fits the redshift evolution of that same luminosity for the same galaxies. The resulting B ∝ (1+z)^{0.7} is essentially the fitted slope 2.9 divided by 4, i.e., 0.725, so the dynamo conclusion is largely a renaming of the fitted luminosity evolution through an equipartition conversion. Because this is one of the paper's central claims, the partial circularity is significant; other parts of the paper retain independent content, so the score is 6 rather than higher.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The analysis requires per-galaxy fitted spectral indices and amplitudes, plus several empirical calibration constants. The main physical assumptions are the two-component power-law SED model, the AGN-free sample, and the equipartition conversion to magnetic fields. No new particles, forces, or physical entities are introduced.

free parameters (4)
  • Per-galaxy nonthermal spectral index alpha_nt = 0.2 to 1.3, mean 0.75 +/- 0.01
    The main fitted quantity in the Bayesian SED fit; it drives the alpha-z relation, the k-correction, the magnetic field estimates, and the SFR calibrations.
  • Per-galaxy SED amplitudes A'_th and A_nt = Table A2
    Nuisance scaling factors in Eq. (8); the thermal amplitude is consistent with zero for most galaxies.
  • MRC calibration coefficients a and b = a = -0.62, b = 2.89
    Fitted relation in Eq. (10) connecting MRC luminosity to 1.3 and 3 GHz luminosities; quoted without uncertainties.
  • SFR calibration normalizations and slopes = Normalizations 10^-28.9, 10^-30.5, 10^-30.7; slopes 0.78, 0.82, 0.83
    Regression fits in Eqs. (19)-(21) relating TIR-based SFR to radio luminosities; these are the paper's calibration outputs.
assumptions (5)
  • domain assumption Radio SED is the sum of optically thin free-free and a single power-law synchrotron component with alpha_th = 0.1 and no curvature.
    Used in Eq. (1) for all SED fits; galaxies with large low-frequency residuals are excluded rather than modeled with curvature, so the assumption is imposed on the final sample.
  • domain assumption The sample is free of significant AGN contamination.
    The sample is inherited from the AGN and red-galaxy exclusion criteria of An et al. 2021; low-luminosity AGNs could in principle flatten the spectra.
  • domain assumption Equipartition between cosmic-ray and magnetic energy densities with K approximately 100 and path length about 1 kpc / cos i.
    Appendix D converts synchrotron luminosity into magnetic field strength; the resulting B values are equipartition estimates, not direct measurements.
  • ad hoc to paper Inclination angles of high-z galaxies are random, so the mean inclination factor is approximately 1.
    States in Sect. 5; the paper notes this leaves up to 0.4 dex uncertainty in B, and orientation-dependent selection is not modeled.
  • domain assumption Galaxy size scales with stellar mass as R_e proportional to M*^0.2.
    Used in Appendix D to convert flux ratios to luminosity ratios; taken from van der Wel et al. 2014 and Du et al. 2024.

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Cite this review

Pith. "Pith review of The Radio Spectral Energy Distribution and Star Formation Calibration in MIGHTEE-COSMOS Highly Star-Forming Galaxies at 1.5 < z < 3.5." pith.science (2026). https://pith.science/paper/EU22GN2X

@misc{pith2026250616275,
  author       = {Pith},
  title        = {Pith review of: The Radio Spectral Energy Distribution and Star Formation Calibration in MIGHTEE-COSMOS Highly Star-Forming Galaxies at 1.5 < z < 3.5},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/EU22GN2X}},
  note         = {Machine review of arXiv:2506.16275}
}
read the original abstract

Studying the radio spectral energy distribution (SED) of distant galaxies is essential for understanding their assembly and evolution over cosmic time. We present rest-frame radio SEDs of a sample of 160 starburst galaxies at redshifts 1.5 to 3.5 in the COSMOS field, as part of the MeerKAT International GHz Tiered Extragalactic Exploration (MIGHTEE) project. MeerKAT observations, combined with archival VLA and GMRT data, allow us to determine the integrated mid-radio (1-10 GHz) continuum (MRC) luminosity and magnetic field strength. A Bayesian method is used to model the SEDs and separate free-free and synchrotron emission. We calibrate the star formation rate (SFR) in radio both directly through SED analysis and indirectly via the infrared-radio correlation (IRRC). With a mean synchrotron spectral index of approximately 0.7, we find that the index flattens with redshift and specific SFR, suggesting that cosmic rays are more energetic in the early universe due to higher star formation activity. The magnetic field strength increases with redshift (B is proportional to (1 + z)^0.7) and with star formation rate (B is proportional to SFR^0.3), indicating a small-scale dynamo as the dominant amplification mechanism. Accounting for SED evolution, the IRRC remains redshift-invariant and does not vary with stellar mass at 1.5 < z < 3.5, though the correlation deviates from linearity. Similarly, we show that SFR estimates based on integrated MRC luminosity are also redshift-invariant.

Figures

Figures reproduced from arXiv: 2506.16275 by the authors.

Figure 1
Figure 1. Star formation rate (SFR) against stellar [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Corner plots showing the two-dimensional posterior probability distribution function (PDF) of [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Radio continuum SEDs at rest-frame (rest-frame flux vs. rest-frame frequency) and their 84% confidence [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figures from the paper (11 more)
Figure 4
Figure 4. Figure 4: Histogram distribution of the non-thermal [PITH_FULL_IMAGE:figures/full_fig_p008_4.png]
Figure 6
Figure 6. Figure 6: A histogram distribution of the equiparti [PITH_FULL_IMAGE:figures/full_fig_p009_6.png]
Figure 7
Figure 7. Figure 7: Nonthermal spectral index αnt against redshift z (a) and specific star formation rate sSFR (b) for SFGs located at 1.5 < z < 3.5. Curves show best fits to the mean values in redshift bins of 0.2 (red points) with their Pearson correlation coefficients rp. Gray shaded a…
Figure 8
Figure 8. Figure 8: Cosmic evolution of the magnetic field strength B of the SFGs at 1 [PITH_FULL_IMAGE:figures/full_fig_p012_8.png]
Figure 9
Figure 9. Figure 9: The IRRC correlation (q-parameter) obtained using the variable αnt (a) or assuming a fixed αnt = 0.7 (b) against redshift z. Panel (c) is the same as panel (a) but with the MRC used instead of the monochromatic radio luminosity at 1.3 GHz (qMRC). Dashed lines show the …
Figure 10
Figure 10. Figure 10: The IRRC correlation (q-parameter) against SFR (a), magnetic field (b), and stellar mass (c). The dashed [PITH_FULL_IMAGE:figures/full_fig_p014_10.png]
Figure 11
Figure 11. Figure 11: Left- The star formation rate (SFR) of the MIGHTEE-COSMOS SFGs located at 1.5 < z < 3.5 against their rest-frame 1.3 GHz radio luminosity. Galaxies at 1.5 < z < 2 are indicated in pink and at 2 < z < 4.5 in blue. Lines show the linear regression fits to the entire poi…
Figure 12
Figure 12. Figure 12: The SFR of the MIGHTEE-COSMOS SFGs at 1.5 < z < 3.5 measured using the TIR luminosity against the SFRs calibrated in radio: left- 1.3 GHz, middle- 3 GHz, and right- MRC. Solid lines show the linear regression fits to the data in all panels. The gray shaded areas show …
Figure 13
Figure 13. Figure 13: Cosmic evolution of the radio luminosity at [PITH_FULL_IMAGE:figures/full_fig_p030_13.png]
Figure 14
Figure 14. Figure 14: Histrogram of the nonthermal spectral index [PITH_FULL_IMAGE:figures/full_fig_p031_14.png]
Figure 15
Figure 15. Figure 15: The non-thermal spectral index distribution for different flux density ranges at 1.3 GHz. [PITH_FULL_IMAGE:figures/full_fig_p032_15.png]

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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. A MIGHTEE robust measurement of the star formation rate-radio correlation

    astro-ph.GA 2026-07 conditional novelty 7.0 of 10

    The SFR–1.4 GHz radio correlation is log10(SFR) = 0.790(L′)+1.244(1+z)^0.122−0.033M′ with 0.178 dex scatter, showing significant redshift but weak mass dependence when AGN are treated probabilistically.

Reference graph

Works this paper leans on

8 extracted references · 7 canonical work pages · cited by 1 Pith paper

  1. [1]

    2013, A&A, 555, A23, doi: 10.1051/0004-6361/201220226 Algera, H

    Adebahr, B., Krause, M., Klein, U., et al. 2013, A&A, 555, A23, doi: 10.1051/0004-6361/201220226 Algera, H. S. B., Smail, I., Dudzeviˇ ci¯ ut˙ e, U., et al. 2020, ApJ, 903, 138, doi: 10.3847/1538-4357/abb77b An, F., Vaccari, M., Smail, I., et al. 2021, MNRAS, 507, 2643, doi: 10.1093/mnras/stab2290 Appleton, P. N., Fadda, D. T., Marleau, F. R., et al. 2004...

    arXiv 2013

  2. [5]

    2022; Laigle et al

    2 Photometric Redshift from COSMOS Catalogues (Weaver et al. 2022; Laigle et al

    work page 2022

  3. [6]

    26 Tabatabaei et al. 43 525980 2.1 0.39 0.18 0.15 − 40.44 30.70 0.21 0.17 30.55 0.21 0.17 44 526965 1.6 1.11 0.13 0.12 − 40.28 30.84 0.07 0.07 30.44 0.07 0.07 45 529975 2.5 0.78 0.19 0.17 − 40.72 31.15 0.12 0.12 30.87 0.12 0.12 46 533924 3.1 0.69 0.11 0.13 − 41.09 31.49 0.09 0.10 31.24 0.09 0.10 47 540343 2.9 1.01 0.12 0.13 − 40.36 30.89 0.07 0.07 30.52 0...

    work page 2015

  4. [8]

    c2 l c3   1 αnt + 3 , (D5) where K is the ratio between the number densities of cosmic-ray protons and electrons and K ′ = K + 1 with K the ratio between the number densities of cosmic-ray protons and electrons. I nt is the nonthermal inten- sity in erg s −1 cm−2 Hz−1 sr−1, αnt is the mean synchrotron spectral index, l is pathlength through the non- th...

    work page 2005

  5. [9]

    For a uniform field with a constant inclination i with respect to the sky plane ( i = 0 ◦ is the face-on view), c3 = [cos(i)](1+αnt)

    )Γ[ 3αnt + 1 6 ] × Γ[ 3αnt + 5 6 ], c4 = √ 3 e3 4πmec2 = 1.86558 × 10−23 erg sr−1 G−1 (D6) in which Γ is the mathematical gamma function. For a uniform field with a constant inclination i with respect to the sky plane ( i = 0 ◦ is the face-on view), c3 = [cos(i)](1+αnt). For dominant synchrotron cooling of the cosmic ray electrons, Eq. (D5) is reduced to ...

    work page 2014

  6. [2016]

    i Photometric Redshift from COSMOS 2020 Catalogue (Weaver et al

    work page 2020

  7. [2019]

    with the MIGHTEE continuum survey. The FMOS-COSMOS is a large near-infrared (NIR) spectroscopic survey of star- forming galaxies and AGNs in the COSMOS field with the Fiber-Multi Object Spectrograph (FMOS) mounted on the Subaru Telescope. The FMOS H band spectral window covers the spectral range of 1.6-1.8 µm to detect the rest-frame Hα and [NII]λ6584 lin...

    work page 2006

  8. [2022]

    ii Photometric Redshift from COSMOS 2015 Catalogue (Laigle et al

    work page 2015

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