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arxiv: 2510.20664 · v2 · submitted 2025-10-23 · 🌌 astro-ph.CO · astro-ph.HE

Niebla: an open-source code for modeling the extragalactic background light

Sara Porras-Bedmar , Manuel Meyer This is my paper

Pith reviewed 2026-05-18 04:24 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.HE
keywords extragalactic background lightEBL modelinggamma-ray attenuationdust re-emissionopen-source codeVHE gamma raysblazar spectra
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The pith

Niebla is an open-source code that models the extragalactic background light using stellar evolution and dust re-emission to show its effect on very-high-energy gamma-ray spectra.

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

The paper introduces Niebla, the first open-source code to compute the extragalactic background light from optical to far-infrared wavelengths with fully customizable inputs. It evolves the spectrum of a single stellar population as a function of redshift using mean metallicity and star formation rate density to model stellar emission, then applies interstellar dust absorption followed by re-emission in the infrared through options such as spectral templates or blackbody combinations. Optional user-provided contributions include stripped stars, intra-halo light, and axion dark matter decay. Three EBL models fitted to observational data are supplied, and a simulation of the blazar Markarian 501 observed with the LHAASO array demonstrates that the very-high-energy spectrum is highly sensitive to the photon density of the EBL at infrared wavelengths.

Core claim

Niebla computes the EBL by evolving a single stellar population spectrum with redshift, mean metallicity and star-formation-rate density, then absorbs the optical emissivity with dust and re-emits it in the infrared using multiple prescriptions. Three resulting EBL models fitted to data are presented, and a simulated LHAASO observation of Markarian 501 in a high-flux state shows that the VHE spectrum is highly sensitive to infrared EBL photon density, enabling distinction between dust reemission models and constraints on EBL parameters with future observations.

What carries the argument

The Niebla code, which generates EBL photon density by evolving single stellar population spectra and applying selectable dust re-emission prescriptions to determine gamma-ray optical depth.

If this is right

  • Future VHE gamma-ray observations can distinguish between different dust re-emission models.
  • EBL parameters can be constrained using data from instruments such as LHAASO.
  • The code enables detailed modeling of EBL optical depth effects on gamma-ray spectra.
  • Users can add extra EBL sources such as axion decay or intra-halo light to test their influence.

Where Pith is reading between the lines

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

  • The infrared sensitivity may allow gamma-ray data to indirectly test dust properties at high redshift.
  • Open availability of the code supports community refinement of EBL models as more observations accumulate.
  • The framework could extend to other high-energy processes attenuated by background photon fields.

Load-bearing premise

The single stellar population evolution with mean metallicity and star-formation-rate density, together with the chosen dust re-emission prescriptions, sufficiently captures the true EBL without major unaccounted contributions or incorrect evolution assumptions.

What would settle it

A measured very-high-energy spectrum from a blazar such as Markarian 501 whose attenuation does not match predictions from any of the provided dust re-emission models at infrared wavelengths.

Figures

Figures reproduced from arXiv: 2510.20664 by Manuel Meyer, Sara Porras-Bedmar.

Figure 1
Figure 1. Figure 1: FIG. 1. Set of synthetic spectra for dust reemission from [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Synthetic spectra of dust emission in the infrared for [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Overview of the EBL measurements used in this analysis. Data have been taken from Hill et al. [ [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. The SFRD as a function of redshift, with the 1 [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. The mean metallicity [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Flare from Markarian 501 in 1997, observed with HEGRA. Data points are taken from the original [ [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. Likelihood ratios of 1000 pseudo-experiments fitting Poissonian draws based on the HEGRA spectrum from the [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9. Best-fit parameters for the 1000 Poissonian pseudo-experiments assuming [PITH_FULL_IMAGE:figures/full_fig_p012_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: FIG. 10. EBL spectral shape for different redshifts. We provide the evolution for our three EBL models (straight lines), as well [PITH_FULL_IMAGE:figures/full_fig_p016_10.png] view at source ↗
read the original abstract

The flux of extragalactic gamma rays is attenuated through interactions with optical and infrared photons of the extragalactic background light (EBL). The EBL is an isotropic, diffuse photon field that is difficult to measure directly at these wavelengths due to strong foreground emission. We present niebla, the first open-source code to compute the EBL from optical to far-infrared wavelengths using a phenomenological approach that accepts fully customizable inputs. This software enables a detailed modeling of the influence of EBL optical depth on gamma-ray observations and facilitates the distinction between different dust reemission models. The code models the optical background primarily from stellar emission, by evolving the spectrum of a single stellar population as a function of redshift, considering mean metallicity evolution and star formation rate density. Additional sources to the EBL can be provided by the user. The code already includes optional contributions from, e.g., stripped stars, intra-halo light, or the decay of axion dark matter. The optical emissivity is then absorbed by interstellar dust and reemitted in the infrared regime. We provide multiple prescriptions to model this process, using spectral dust templates or a combination of blackbodies. We provide three EBL models calculated with different dust reemission prescriptions, which have been fitted to various observational data sets. In addition, we showcase the versatility of our model through a simulated observation of the blazar Markarian 501 in a high-flux state with the LHAASO array. We find that the simulated VHE spectrum is highly sensitive to the photon density of the EBL at infrared wavelengths. Our model will therefore allow the community to distinguish between different dust reemission models and constrain EBL parameters with future observations.

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

1 major / 3 minor

Summary. The manuscript introduces niebla, the first open-source code for computing the extragalactic background light (EBL) from optical to far-infrared wavelengths via a phenomenological model. Optical emissivity is generated by evolving a single stellar population spectrum with mean metallicity evolution and a star-formation rate density SFRD(z); this emissivity is absorbed by dust and re-emitted in the IR using user-selectable prescriptions (spectral templates or blackbody combinations). Three specific EBL models are supplied after fitting to observational data sets, with optional user-added components such as stripped stars, intra-halo light, or axion decay. The code is demonstrated through a simulated LHAASO observation of the blazar Markarian 501 in a high state, where the VHE spectrum is shown to be sensitive to the IR EBL photon density; the authors conclude that the framework will enable the community to distinguish dust re-emission models and constrain EBL parameters with future observations.

Significance. If the modeling assumptions are shown to be robust, niebla would provide a valuable, customizable open-source tool for gamma-ray astrophysics and cosmology, allowing reproducible exploration of EBL attenuation effects on VHE spectra. The provision of multiple dust prescriptions, fully customizable inputs, and optional non-stellar contributions (e.g., axion decay) are clear strengths that facilitate community use and falsifiable tests. The LHAASO simulation illustrates practical utility for future observations. Significance is reduced, however, until the relative size of systematics from the single-population stellar modeling versus dust-model variations is quantified.

major comments (1)
  1. [§2] §2 (Phenomenological modeling of stellar emission): The adoption of a single stellar population evolved with mean metallicity and a single SFRD(z) to generate optical emissivity omits the dispersion in star-formation histories, metallicities, and dust geometries across the galaxy population. Because the VHE attenuation kernel is most sensitive in the 10–100 µm range, any resulting systematic offset in the absorbed energy budget and IR photon density could be comparable to the template-to-blackbody variations highlighted in the three EBL models. This directly affects the central claim (abstract and §4 simulation) that future LHAASO-type spectra will cleanly separate the dust re-emission models; a quantitative comparison to multi-population or semi-analytic EBL calculations is needed to establish that the dust-model differences exceed these systematics.
minor comments (3)
  1. [Abstract and §3] Abstract and §3 (fitting procedure): No quantitative validation metrics (e.g., χ² values, residual plots, or posterior uncertainties) are reported for the fits of the three EBL models to the observational data sets; this makes it difficult to assess how post-hoc choices in dust parameters propagate into the final photon densities.
  2. [§4] §4 (LHAASO simulation): The simulated VHE spectrum sensitivity is presented without error bands arising from stellar-model uncertainties or from the fitting procedure; adding these would clarify whether the dust-model separation remains distinguishable.
  3. Code and data availability: While the manuscript states that niebla is open-source, the repository link, version number, and exact input files used for the three published EBL models should be provided to ensure full reproducibility.

Simulated Author's Rebuttal

1 responses · 1 unresolved

We thank the referee for their constructive review and for highlighting an important limitation in our phenomenological modeling approach. We address the major comment in detail below, have revised the manuscript to incorporate appropriate caveats and clarifications, and note one aspect that remains a standing limitation.

read point-by-point responses

  1. Referee: [§2] §2 (Phenomenological modeling of stellar emission): The adoption of a single stellar population evolved with mean metallicity and a single SFRD(z) to generate optical emissivity omits the dispersion in star-formation histories, metallicities, and dust geometries across the galaxy population. Because the VHE attenuation kernel is most sensitive in the 10–100 µm range, any resulting systematic offset in the absorbed energy budget and IR photon density could be comparable to the template-to-blackbody variations highlighted in the three EBL models. This directly affects the central claim (abstract and §4 simulation) that future LHAASO-type spectra will cleanly separate the dust re-emission models; a quantitative comparison to multi-population or semi-analytic EBL calculations is needed to establish that the dust-model differences exceed these systematics.

    Authors: We agree that the single stellar population with mean metallicity and a single SFRD(z) is a simplification that does not capture the full dispersion in star-formation histories, metallicities, and dust geometries present in the real galaxy population. This choice was made to keep the model computationally lightweight, fully customizable, and focused on the dust re-emission component, which is the primary novelty of the code. The manuscript already emphasizes that additional non-stellar contributions can be added by the user; the same modular structure allows replacement or extension of the stellar emissivity module. In the revised version we have added an explicit limitations paragraph in §2 and a corresponding caveat in §4 and the abstract, stating that the reported differences between the three dust prescriptions are shown under the adopted single-population stellar assumptions and that systematic uncertainties arising from stellar-population dispersion could affect the absolute IR photon density at a level comparable to or larger than the template variations. We have also revised the language of the central claim to indicate that the framework enables the community to explore and distinguish dust re-emission models once the stellar modeling uncertainties are separately quantified or marginalized. A full quantitative error-budget comparison against multi-population or semi-analytic EBL calculations (e.g., those based on GALFORM or other SAMs) would require new integrations and is not performed in the present work. revision: partial

standing simulated objections not resolved
  • Quantitative comparison of the single-population EBL models against multi-population or semi-analytic calculations, including a direct assessment of whether dust-model differences exceed stellar-population systematics in the 10–100 µm range relevant for VHE attenuation.

Circularity Check

0 steps flagged

No significant circularity in the phenomenological EBL modeling chain

full rationale

The niebla framework is explicitly constructed as a customizable, open-source code that accepts arbitrary user inputs for stellar population evolution, metallicity, SFRD, dust re-emission prescriptions, and optional additional components. The three provided EBL models are stated to have been fitted to observational datasets, but this is presented as an application of the tool rather than a derivation that reduces to its own inputs by construction. The simulated VHE spectrum for Markarian 501 is a forward-modeling exercise demonstrating sensitivity to IR photon density; it does not constitute a tautological prediction forced by prior fits. No self-definitional equations, load-bearing self-citations, uniqueness theorems, or ansatz smuggling appear in the described methodology. The derivation from single-population emissivity through dust absorption/re-emission remains independent and falsifiable against external data.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 0 invented entities

The central modeling rests on standard astrophysical assumptions about stellar populations and dust, plus several parameters that are either chosen or fitted to data to produce the three EBL models.

free parameters (3)
  • star formation rate density evolution
    Used to evolve the spectrum of a single stellar population as a function of redshift
  • mean metallicity evolution parameters
    Incorporated when evolving the stellar emission spectrum
  • dust re-emission template or blackbody parameters
    Adjusted when fitting the three EBL models to observational data sets
axioms (2)
  • domain assumption Optical background is modeled primarily from evolving stellar emission
    Core phenomenological approach described in the abstract
  • domain assumption Optical emissivity is absorbed by interstellar dust and re-emitted in the infrared
    Standard assumption for connecting optical and infrared EBL components

pith-pipeline@v0.9.0 · 5842 in / 1683 out tokens · 49767 ms · 2026-05-18T04:24:10.905165+00:00 · methodology

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Works this paper leans on

66 extracted references · 66 canonical work pages · 5 internal anchors

  1. [1]

    The time scale for this creation is of the order of 10 7 years, which can be ap- proximated as instantaneous in cosmic terms

    Stellar contribution A simple stellar population (SSP) is a group of stars born from a single gas cloud. The time scale for this creation is of the order of 10 7 years, which can be ap- proximated as instantaneous in cosmic terms. Following this first burst no more star formation occurs. The emis- sivity of a stellar population can be calculated as ενstel...

    work page

  2. [2]

    These stars would create a faint halo surrounding their host galaxies, but would not have been used to calculate the ρ⋆

    Intra-halo light The IHL is the light caused by stars that have been ejected from their galaxies by dynamical events. These stars would create a faint halo surrounding their host galaxies, but would not have been used to calculate the ρ⋆. We follow the parametrization described by Bernal et al. [8] to calculate the emissivity ελ,IHL(λ, z) = Z Mmax Mmin dn...

    work page

  3. [3]

    In contrast to axions, ALPs do not solve the strong CP problem and their massm a is independent of the coupling constant to photonsg aγ

    Cosmic ALP decay Axions are hypothetical pseudo-Nambu-Goldstone bosons, which are a consequence of the Peccei-Quinn so- lution to the strong CP problem in QCD. In contrast to axions, ALPs do not solve the strong CP problem and their massm a is independent of the coupling constant to photonsg aγ. Both axions and ALPs are candidates to make up cold dark mat...

    work page

  4. [4]

    Additional contributions to the COB could come, e.g., from AGN as their spectra span the entire electromag- netic spectrum

    Other contributions The list of sources introduced above is not exhaustive. Additional contributions to the COB could come, e.g., from AGN as their spectra span the entire electromag- netic spectrum. However their contribution to the EBL intensity is as low as∼10% of the stellar one [5, 34]. We do not include a parametrization for this source in niebla. H...

    work page

  5. [5]

    TheCharyspectral models are normalized to the total luminosity of ULIRGs

    Spectral templates The first library we use is a set of synthetic galactic spectra derived from observations of ultra luminous in- frared galaxies (ULIRGs) [13], which we refer to asChary from here on. TheCharyspectral models are normalized to the total luminosity of ULIRGs. We need to rescale them to the luminosity of a single SSP, which we do by introdu...

    work page

  6. [6]

    For example, poly- cyclic aromatic hydrocarbon and very small grains are heated in galaxies toT∼ O(100 K), and therefore emit in the mid infrared (MIR) [13, 20]

    Black body spectra The second method to calculate the infrared emission assumes different dust populations, where the reemitted light follows a black-body spectrum for each population peaking at different temperatures. For example, poly- cyclic aromatic hydrocarbon and very small grains are heated in galaxies toT∼ O(100 K), and therefore emit in the mid i...

    work page

  7. [7]

    The metallicity evolution is taken from Tanikawa et al

    to parametrize the SFRD. The metallicity evolution is taken from Tanikawa et al. [55]. We assume the same functional form for the dust absorption as Finke et al. [20]. The mathematical formulas for these models are compiled in Appendix A. Each of the dust reemission models has a different number of free parameters. We introduce two free pa- rameters forCh...

    work page 2004

  8. [8]

    Quantum Universe

    to characterize the detector. A flare in the energy range between a few hundred GeV and 20 TeV would be observed with the water Cherenkov detector array (WCDA), which is sensitive to energies 100 GeV-30 TeV. The number of counts that would be observed is given by µ(∆Eobs) = ∆T Z ∆Eobs dEobs × Z ∞ 0 R(E obs, Etrue)A eff (Etrue)ϕ(E true)dE true, (18) where ...

    work page 1997

  9. [9]

    Abdalla, H., Abe, H., Acero, F., et al. 2021, J. Cosmology Astropart. Phys., 2021, 048

    work page 2021

  10. [10]

    2012, Sci- ence, 338, 1190

    Ackermann, M., Ajello, M., Allafort, A., et al. 2012, Sci- ence, 338, 1190

    work page 2012

  11. [11]

    A., Akhperjanian, A

    Aharonian, F. A., Akhperjanian, A. G., Barrio, J. A., et al. 1999, A&A, 349, 11

    work page 1999

  12. [12]

    A., Akhperjanian, A

    Aharonian, F. A., Akhperjanian, A. G., Barrio, J. A., et al. 2001, A&A, 366, 62

    work page 2001

  13. [13]

    K., Driver, S

    Andrews, S. K., Driver, S. P., Davies, L. J. M., Lagos, C. d. P., & Robotham, A. S. G. 2017, Monthly Notices of the Royal Astronomical Society, 474, 898

    work page 2017

  14. [14]

    J., & Scott, P

    Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481

    work page 2009

  15. [15]

    2022, Chinese Physics C, 46, 035001

    Bai, X., Bi, B., Bi, X., et al. 2022, Chinese Physics C, 46, 035001

    work page 2022

  16. [16]

    L., Caputo, A., Sato-Polito, G., Mirocha, J., & Kamionkowski, M

    Bernal, J. L., Caputo, A., Sato-Polito, G., Mirocha, J., & Kamionkowski, M. 2023, Phys. Rev. D, 107, 103046

    work page 2023

  17. [17]

    A., & Biteau, J

    Biasuzzi, B., Hervet, O., Williams, D. A., & Biteau, J. 2019, A&A, 627, A110

    work page 2019

  18. [18]

    2023, The Multi-Messenger Extragalactic Spectrum

    Biteau, J. 2023, The Multi-Messenger Extragalactic Spectrum

    work page 2023

  19. [19]

    & Williams, D

    Biteau, J. & Williams, D. A. 2015, ApJ, 812, 60

    work page 2015

  20. [20]

    & Salim, S

    Boquien, M. & Salim, S. 2021, A&A, 653, A149

    work page 2021

  21. [21]

    & Elbaz, D

    Chary, R. & Elbaz, D. 2001, ApJ, 556, 562

    work page 2001

  22. [22]

    S., Agudo, I., et al

    Cherenkov Telescope Array Consortium, Acharya, B. S., Agudo, I., et al. 2019, Science with the Cherenkov Tele- scope Array

    work page 2019

  23. [23]

    2011, European Physical Journal C, 71, 1554

    Cowan, G., Cranmer, K., Gross, E., & Vitells, O. 2011, European Physical Journal C, 71, 1554

    work page 2011

  24. [24]

    de Matos Pimentel, D. R. & Moura-Santos, E. 2019, J. Cosmology Astropart. Phys., 2019, 043

    work page 2019

  25. [25]

    Dembinski, H. et al. 2020

    work page 2020

  26. [26]

    P., Andrews, S

    Driver, S. P., Andrews, S. K., Davies, L. J., et al. 2016, The Astrophysical Journal, 827, 108, aDS Bibcode: 2016ApJ...827..108D

    work page 2016

  27. [27]

    2018, Science, 362, 1031

    Fermi-LAT Collaboration, Abdollahi, S., Ackermann, M., et al. 2018, Science, 362, 1031

    work page 2018

  28. [28]

    D., Ajello, M., Dom´ ınguez, A., et al

    Finke, J. D., Ajello, M., Dom´ ınguez, A., et al. 2022, ApJ, 941, 33

    work page 2022

  29. [29]

    D., Razzaque, S., & Dermer, C

    Finke, J. D., Razzaque, S., & Dermer, C. D. 2010, ApJ, 712, 238

    work page 2010

  30. [30]

    & Rocca-Volmerange, B

    Fioc, M. & Rocca-Volmerange, B. 2019, Astronomy & Astrophysics, 623, A143

    work page 2019

  31. [31]

    Forbes, D. A. & Ponman, T. J. 1999, Monthly Notices of the Royal Astronomical Society, 309, 623

    work page 1999

  32. [32]

    & Rodighiero, G

    Franceschini, A. & Rodighiero, G. 2017, A&A, 603, A34

    work page 2017

  33. [33]

    2008, A&A, 487, 837

    Franceschini, A., Rodighiero, G., & Vaccari, M. 2008, A&A, 487, 837

    work page 2008

  34. [34]

    Gould, R. J. & Schr´ eder, G. P. 1967, Physical Review, 155, 1408

    work page 1967

  35. [35]

    Gould, R. J. & Schr´ eder, G. P. 1967, Physical Review, 155, 1404

    work page 1967

  36. [36]

    2024, The Astrophysical Journal Letters, 975, L18

    Gr´ eaux, L., Biteau, J., & Nievas Rosillo, M. 2024, The Astrophysical Journal Letters, 975, L18

    work page 2024

  37. [37]

    E., Groh, J

    G¨ otberg, Y., de Mink, S. E., Groh, J. H., Leitherer, C., & Norman, C. 2019, A&A, 629, A134

    work page 2019

  38. [38]

    H. E. S. S. Collaboration, Abramowski, A., Acero, F., et al. 2013, A&A, 550, A4

    work page 2013

  39. [39]

    & Madau, P

    Haardt, F. & Madau, P. 2012, The Astrophysical Journal, 746, 125, aDS Bibcode: 2012ApJ...746..125H

    work page 2012

  40. [40]

    G., Arendt, R

    Hauser, M. G., Arendt, R. G., Kelsall, T., et al. 1998, ApJ, 508, 25

    work page 1998

  41. [41]

    The Spectrum of the Universe

    Hill, R., Masui, K. W., & Scott, D. 2018, Applied Spec- troscopy, 72, 663, arXiv:1802.03694 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  42. [42]

    & Srianand, R

    Khaire, V. & Srianand, R. 2019, Monthly Notices of the Royal Astronomical Society, 484, 4174

    work page 2019

  43. [43]

    Kneiske, T. M. & Dole, H. 2010, Astronomy and Astro- physics, 515, A19, arXiv:1001.2132 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  44. [44]

    M., Mannheim, K., & Hartmann, D

    Kneiske, T. M., Mannheim, K., & Hartmann, D. H. 2002, Astronomy & Astrophysics, 386, 1, arXiv:astro- ph/0202104

    work page arXiv 2002

  45. [45]

    2002, Science, 295, 82

    Kroupa, P. 2002, Science, 295, 82

    work page 2002

  46. [46]

    2014, The Astrophysical Journal Supplement Series, 212, 14, aDS Bibcode: 2014ApJS..212...14L

    Leitherer, C., Ekstr¨ om, S., Meynet, G., et al. 2014, The Astrophysical Journal Supplement Series, 212, 14, aDS Bibcode: 2014ApJS..212...14L

    work page 2014

  47. [47]

    D., et al

    Leitherer, C., Schaerer, D., Goldader, J. D., et al. 1999, The Astrophysical Journal Supplement Series, 123, 3, aDS Bibcode: 1999ApJS..123....3L

    work page 1999

  48. [48]

    Cosmic Star Formation History

    Madau, P. & Dickinson, M. 2014, Annual Review of Astronomy and Astrophysics, 52, 415, arXiv:1403.0007 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  49. [49]

    G., Pyo, J., & Tsumura, K

    Matsumoto, T., Kim, M. G., Pyo, J., & Tsumura, K. 2015, ApJ, 807, 57

    work page 2015

  50. [50]

    J., et al

    Matsuura, S., Arai, T., Bock, J. J., et al. 2017, The As- trophysical Journal, 839, 7, publisher: The American As- tronomical Society

    work page 2017

  51. [51]

    2022, ebltable

    Meyer, M. 2022, ebltable

    work page 2022

  52. [52]

    2012, A&A, 542, A59

    Meyer, M., Raue, M., Mazin, D., & Horns, D. 2012, A&A, 542, A59

    work page 2012

  53. [53]

    L., & Bressan, A

    Moll´ a, M., Garc´ ıa-Vargas, M. L., & Bressan, A. 2009, MNRAS, 398, 451

    work page 2009

  54. [54]

    G., Power, C., & Robotham, A

    Murray, S. G., Power, C., & Robotham, A. S. G. 2013, Astronomy and Computing, 3, 23

    work page 2013

  55. [55]

    1962, JETP, 14, No

    Nikishov, A. 1962, JETP, 14, No. 2, 393

    work page 1962

  56. [56]

    Overduin, J. M. & Wesson, P. S. 2004, Physics Reports, 402, 267, arXiv:astro-ph/0407207

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  57. [57]

    & Howk, J

    P´ eroux, C. & Howk, J. C. 2020, ARA&A, 58, 363 14

    work page 2020

  58. [58]

    2024, Phys

    Porras-Bedmar, S., Meyer, M., & Horns, D. 2024, Phys. Rev. D, 110, 103501

    work page 2024

  59. [59]

    R., Parker, J

    Postman, M., Lauer, T. R., Parker, J. W., et al. 2024, arXiv e-prints, arXiv:2407.06273

    work page arXiv 2024

  60. [60]

    Probing the peak of the star formation rate density with the extragalactic background light

    Raue, M. & Meyer, M. 2012, Monthly Notices of the Royal Astronomical Society, 426, 1097, arXiv:1203.0310 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  61. [61]

    D., & Finke, J

    Razzaque, S., Dermer, C. D., & Finke, J. D. 2009, The Astrophysical Journal, 697, 483

    work page 2009

  62. [62]

    G., et al

    Saldana-Lopez, A., Dom´ ınguez, A., P´ erez-Gonz´ alez, P. G., et al. 2021, Monthly Notices of the Royal Astro- nomical Society, 507, 5144, arXiv:2012.03035 [astro-ph]

    work page arXiv 2021

  63. [63]

    2022, ApJ, 926, 83

    Tanikawa, A., Yoshida, T., Kinugawa, T., et al. 2022, ApJ, 926, 83

    work page 2022

  64. [64]

    E., et al

    Veale, M., Ma, C.-P., Greene, J. E., et al. 2017, Monthly Notices of the Royal Astronomical Society, 473, 5446

    work page 2017

  65. [65]

    A., Cohen, S

    Windhorst, R. A., Cohen, S. H., Jansen, R. A., et al. 2023, The Astronomical Journal, 165, 13 Appendix A: Parametrizations already listed in the EBL code We present a list of all the parametrizations present in the EBL code in Table V. The possibility to input custom parameters and functions is also available for all the expressions that we list here. App...

    work page 2023

  66. [66]

    We also share the dust absorption methodol- ogy, so the spectral shapes are very similar in the optical regime

    use. We also share the dust absorption methodol- ogy, so the spectral shapes are very similar in the optical regime. Moreover, our 2BB model shares their methodol- ogy of dust reemission in the MIR, so these two are sim- ilar in this regime. Saldana-Lopez et al. [54] derive the EBL from observed spectral energy densities of galaxies without fits to the ac...

    work page 1997