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arxiv: 2606.13351 · v1 · pith:FGGK5XXRnew · submitted 2026-06-11 · 🌌 astro-ph.SR

Stellar Population Spectra Incorporating Detailed Binary Evolution using POSYDON

Eirini Kasdagli , Jeff J. Andrews , Bret Lehmer , Rich Townsend , Manor Zapartas , Andreas Zezas , Max Briel , Tassos Fragos
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Seth Gossage Philipp M. Srivastava Elizabeth Teng
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Pith reviewed 2026-06-27 05:40 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords stellar populationsbinary evolutionspectral synthesisionizing photonsstripped starsWolf-Rayet starsultraviolet spectra
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The pith

Binary interactions cause stripped stars to dominate the ionizing spectra of stellar populations after about 16 million years.

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

This paper creates new spectral models for groups of stars that account for how stars interact in binaries. It shows that these interactions change the light output in ultraviolet and high-energy ionizing wavelengths in important ways. Early on, massive Wolf-Rayet stars produce most of the ionizing light, but after roughly 16 million years, stars that have been stripped of their outer layers through mass transfer become the main source. The production of specific helium-ionizing photons proves particularly dependent on these stripped stars. The models are released publicly to help improve estimates of star formation and other properties from observed spectra.

Core claim

The inclusion of binary interactions has a significant effect on the UV and ionizing regime of the integrated spectrum. Wolf-Rayet and massive stars dominate the production of ionizing radiation at earlier times, but after about 16 million years stripped stars produced through mass transfer begin to dominate. The production of ionizing He II photons is especially sensitive to the underlying population of stripped stars.

What carries the argument

Spectral synthesis using binary population synthesis that incorporates dedicated libraries for Wolf-Rayet stars, stripped helium stars from mass transfer, and stellar mergers.

Load-bearing premise

The binary population synthesis code and selected spectral libraries correctly represent the evolutionary outcomes and spectra of massive stars undergoing binary interactions at solar metallicity.

What would settle it

Spectroscopic observations of star-forming regions with ages between 15 and 30 million years that show no excess in He II ionizing flux compared to single-star predictions would indicate that the stripped-star contribution is overstated.

Figures

Figures reproduced from arXiv: 2606.13351 by Andreas Zezas, Bret Lehmer, Eirini Kasdagli, Elizabeth Teng, Jeff J. Andrews, Manor Zapartas, Max Briel, Philipp M. Srivastava, Rich Townsend, Seth Gossage, Tassos Fragos.

Figure 1
Figure 1. Figure 1: The flow chart outlining our procedure for identifying from which library each star’s synthetic spectrum will be generated, based on its input parameter such as log g, Teff and XH. Spectra for H-poor stars, with surface XH < 0.6 like WR stars and stripped stars, are drawn from bespoke spectral libraries. For hot stars, we use either the OSTAR or BSTAR grids depending on Teff (Lanz & Hubeny 2003, 2007), whi… view at source ↗
Figure 2
Figure 2. Figure 2: The spectral energy distribution of our fiducial stellar population model over time including binaries. The populations span a range of ages from 1 Myr to 1 Gyr. WR stars produce the bulk of the Lyman continuum (LyC) radiation (λ < 912 ˚A), while O- and B-type stars dominate the UV continuum (λ > 912 ˚A). As the pop￾ulation ages, massive stars evolve off the MS to become red supergiants. As a consequence, … view at source ↗
Figure 3
Figure 3. Figure 3: We show the spectra from binary and single star populations over several ages ranging from 1 Myr to 100 Myr. The binary spectra are plotted in the shades of red, while single star populations are in blue colors. Shortly after 1 Myr, we see a steep drop in the UV radiation from the single stars populations, in stark contrast to binary populations, which continue to emit hard ionizing radiation over time due… view at source ↗
Figure 4
Figure 4. Figure 4: Breakdown of spectral contributions of ionizing and UV-bright sources for several ages ranging from 1 Myr to 100 Myr. We display with different colored lines the contributions from binaries populations such as WR (purple), O-type stars (blue), stripped stars (red) and merged stars (green). We also include the flux of the overall population (black). For populations younger than 15 Myr the WR populations dom… view at source ↗
Figure 5
Figure 5. Figure 5: The number of WR and their species in a star￾burst fiducial model as a function of time. The dashed lines represent the numbers from single star populations. Binary populations are able to produce and sustain relatively large numbers of WR stars over longer periods compared with the single stars. from our population and are only present for the first 10 Myr. Binary interactions are expected to affect the f… view at source ↗
Figure 6
Figure 6. Figure 6: The number of stripped stars in our fiducial pop￾ulation model as a function of time. We break down the for￾mation channels and compare them with the total amount of stripped stars. These formation channels are stripped stars formed from stable case B mass transfer, stable case A mass transfer and stripped stars from post CE systems. We also include stripped stars formed from the secondary star. The majori… view at source ↗
Figure 7
Figure 7. Figure 7: The emission rates of ionizing photons binary and single star populations as a function of time. The solid lines correspond to the emission rates produced by the bi￾nary population and the dashed lines from only single star population. from Dotter (2016) and Choi et al. (2017). We com￾pute the spectral output of the MIST models at several ages by using FSPS (Conroy et al. 2009; Conroy & Gunn 2010). Both ou… view at source ↗
Figure 8
Figure 8. Figure 8: Spectral models of single-star populations at several ages. In the left panel, we compare the POSYDON single-star models with spectral models produced using the MIST evolutionary tracks. In the right panel, we compare the POSYDON single-star models with the BC2019 models. comparing the choices made for key parameters in the MESA simulations. One of these parameters in particu￾lar, convective overshooting, … view at source ↗
Figure 9
Figure 9. Figure 9: We compare our synthetic stellar population spectra at Z⊙ for ages in range of 1 Myr to 126 Myr with single star spectra. The left panel includes spectral models based on the MIST evolutionary tracks, that are colored in green. The right panel has comparisons of the CB2019 models in gray [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of the integrated binary population spectra predicted by our fiducial models and BPASS at selected ages. The red spectra correspond our fiducial binary population models, while the grey show the corresponding BPASS binary spectra at ages of 1, 15, 20, 50, and 100 Myr. Both spectra represent a population of initial stellar mass of 106 . This comparisons illustrates how different assumption about… view at source ↗
Figure 11
Figure 11. Figure 11: The number of stripped stars as a function of time from the POSYDON models (Red line) and the BPASS models (Black line) as a function of age. For reference we include the predictions of stripped stars from G¨otberg et al. (2019), albeit they were produced by a different IMF. and the underlying population of stripped stars. From [PITH_FULL_IMAGE:figures/full_fig_p016_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: The emission rates of ionizing photons from a starburst as a function of time from three different models: POSYDON populations including binaries (solid, orange), BPASS populations including binaries (dashed, green), and single-star MIST (dotted, purple). The POSYDON and BPASS models produce similar amounts of ionizing photons, with some differences present in the QHeII . On the other hand, the MIST spect… view at source ↗
Figure 13
Figure 13. Figure 13: The number of primary H-poor stars for starbursts of 106 M⊙ across a range of ages. We have chosen to separately explore the convergence in two different regimes: one for ages less than 16 Myr (left panel) and one for ages older 16 Myr (right panel). For each age we assume a time binning equal to a percentage of that age. Increasing the bin widths leads to convergence in our predictions of stripped stars.… view at source ↗
Figure 14
Figure 14. Figure 14: Comparison of starburst spectra computed using bin widths to illustrate the effect of time binning on population spectra. The left column shows populations constructed with bin widths ranging from ±10% to 25%, while the right column displays narrower bin widths from ±1% to 10%. We isolate the two wavelength regimes exhibiting the largest spectral variations: the Lyman continuum (LyC) and the infrared (IR)… view at source ↗
Figure 15
Figure 15. Figure 15: We compare spectral models of several ages made with two different methods. The black lines show the spectra of 106M⊙ single star population generated by a combination of stochastic sampling and time-dependent interpolation for the stellar properties. The lines in red are the spectral models for populations of the same stellar mass, that were constructed by weighting the individual spectra of every star i… view at source ↗
read the original abstract

The accuracy of stellar population properties inferred through spectral energy distribution fitting hinges on the reliability of the underlying spectral models. Binary interactions are fundamental for massive star evolution, and ignoring their spectral contribution can lead to incorrect results. We use the POSYDON binary population synthesis code to generate spectral models of stellar populations that include binaries at solar metallicity. Our framework incorporates a collection of spectral libraries that is designed to address key outcomes of binary stellar evolution like Wolf-Rayet stars, stripped helium stars, and a treatment for stellar mergers. Our models confirm previous results showing that the inclusion of binary interactions has a significant effect on the UV and ionizing regime of the integrated spectrum. In particular we find that Wolf-Rayet stars and other massive stars dominate the production of ionizing radiation at earlier times, but after $\simeq$16 Myr stripped stars produced through mass transfer begin to dominate. Furthermore, we show that the production of ionizing He II photons is especially sensitive to the underlying population of stripped stars. While our results currently focus on high-mass stars ($\ge4~M_{\odot}$) at Solar metallicity, they provide the framework for binary spectral synthesis across a range of metallicities and masses and lay the foundation for calculations of the emergent emission-line spectra in the UV, optical, and IR regimes. We make the spectral models from this work publicly available for use in a format that can be integrated into fitting codes.

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 / 2 minor

Summary. The paper presents new spectral synthesis models for stellar populations at solar metallicity generated with the POSYDON binary population synthesis code. These models incorporate dedicated spectral libraries to account for binary-evolution outcomes including Wolf-Rayet stars, stripped helium stars, and merger products. The work confirms that binary interactions substantially alter the UV and ionizing portions of the integrated spectrum, with Wolf-Rayet and massive stars dominating ionizing output at early times but stripped stars produced via mass transfer becoming dominant after ≃16 Myr; He II ionizing photons are shown to be particularly sensitive to the stripped-star population. The models are released publicly in a format suitable for integration into SED-fitting codes, and the framework is positioned for future extension to other metallicities and mass ranges.

Significance. If the POSYDON-derived populations and attached spectral libraries are reliable, the work supplies a concrete, publicly available set of binary-inclusive population spectra that directly addresses a known limitation in current stellar-population modeling. The explicit timeline for the shift in ionizing-photon sources and the demonstrated sensitivity of He II output constitute falsifiable predictions that can be tested against observations of young clusters. The provision of a modular framework for additional metallicities and masses further increases the potential utility for both theoretical studies and observational interpretation.

major comments (2)
  1. [Abstract] Abstract and results section: The headline result that stripped stars overtake Wolf-Rayet/massive stars at ≃16 Myr and dominate He II production is load-bearing on the accuracy of POSYDON’s mass-transfer, common-envelope, and merger prescriptions for stars ≥4 M⊙ at solar metallicity. No direct validation of the predicted stripped-helium-star number densities, lifetimes, or UV/He II continua against observed samples or independent binary codes is reported, leaving the central claim without the quantitative cross-checks required to assess its robustness.
  2. [Methods] Methods: The manuscript states that a “collection of spectral libraries” is used to treat Wolf-Rayet stars, stripped helium stars, and mergers, yet provides no quantitative assessment of how uncertainties in the library assignments (e.g., effective-temperature or wind prescriptions for stripped stars) propagate into the integrated ionizing-photon budgets or the reported 16 Myr transition time.
minor comments (2)
  1. [Abstract] The abstract refers to “high-mass stars (≥4 M⊙)” while the title and introduction emphasize the full binary population; a brief clarification of the mass cut and its justification would improve readability.
  2. Figure captions and text should explicitly state the assumed initial mass function, binary fraction, and period distribution so that readers can reproduce the population synthesis setup without consulting the POSYDON documentation.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed report. Below we provide point-by-point responses to the two major comments. We have revised the manuscript to strengthen the discussion of model assumptions and limitations while preserving the scope of the present work.

read point-by-point responses

  1. Referee: [Abstract] Abstract and results section: The headline result that stripped stars overtake Wolf-Rayet/massive stars at ≃16 Myr and dominate He II production is load-bearing on the accuracy of POSYDON’s mass-transfer, common-envelope, and merger prescriptions for stars ≥4 M⊙ at solar metallicity. No direct validation of the predicted stripped-helium-star number densities, lifetimes, or UV/He II continua against observed samples or independent binary codes is reported, leaving the central claim without the quantitative cross-checks required to assess its robustness.

    Authors: We agree that the reported 16 Myr transition depends on the fidelity of POSYDON’s binary-evolution prescriptions. Those prescriptions were validated against both observations and other binary population synthesis codes in the series of POSYDON methodology papers (explicit citations will be added). The present manuscript applies the already-validated POSYDON populations to spectral synthesis; it does not repeat those validation exercises. In the revised text we will (i) add a dedicated paragraph in the Discussion that explicitly references the prior POSYDON validation studies for stars ≳4 M⊙ at solar metallicity and (ii) state that the timeline and He II sensitivity are predictions that can be tested once the models are compared with observations or other codes. We therefore regard the central claim as resting on published validations rather than being unanchored. revision: partial

  2. Referee: [Methods] Methods: The manuscript states that a “collection of spectral libraries” is used to treat Wolf-Rayet stars, stripped helium stars, and mergers, yet provides no quantitative assessment of how uncertainties in the library assignments (e.g., effective-temperature or wind prescriptions for stripped stars) propagate into the integrated ionizing-photon budgets or the reported 16 Myr transition time.

    Authors: The referee is correct that no quantitative uncertainty propagation from the spectral-library choices is presented. A full Monte-Carlo error budget lies beyond the scope of this first solar-metallicity paper. In the revision we will insert a new subsection (Methods or Discussion) that (a) lists the specific libraries and their adopted T_eff and wind prescriptions for each evolutionary channel, (b) qualitatively discusses how plausible variations in those prescriptions would affect the ionizing-photon budgets, and (c) notes that the 16 Myr transition time is most sensitive to the lifetimes and temperatures assigned to the stripped-helium-star population. This addition will allow readers to gauge the robustness of the reported results without requiring new numerical experiments. revision: yes

Circularity Check

0 steps flagged

No significant circularity; forward models from established codes

full rationale

The paper generates integrated spectra by feeding POSYDON binary population synthesis outputs and attached spectral libraries (for WR stars, stripped He stars, mergers) into a population synthesis framework at solar metallicity for M≥4 M⊙. All reported results, including the transition at ≃16 Myr and He II sensitivity, are direct simulation outputs rather than quantities fitted to the target observables or redefined by construction. No equations, parameter fits, or self-citations are shown that reduce the central claims to their own inputs; the work is self-contained forward modeling whose validity rests on the external accuracy of POSYDON and the libraries, not on internal loops.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on the accuracy of the POSYDON code and the spectral libraries chosen to represent binary-evolution products; no free parameters are explicitly fitted in the abstract, but the models inherit all internal parameters of POSYDON.

axioms (2)
  • domain assumption POSYDON binary population synthesis code accurately models binary evolution at solar metallicity for stars ≥4 M⊙
    The paper relies on this code to generate the underlying stellar populations whose spectra are then computed.
  • domain assumption The selected spectral libraries correctly represent the spectra of Wolf-Rayet stars, stripped helium stars, and merger products
    These libraries are invoked to address key binary outcomes in the integrated spectrum.

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