Muspelheim

These files (zipped) contain rest-frame spectral energy distributions for stars at various ages.

10% solar tracks, 9-575 M_☉, Szécsi et al. (2022): [v1.0] (60 Mb)
Pop III tracks, 10-1000 M_☉, Yoon et al. (2012), no rotation: [v1.0] (26 Mb)
Pop III tracks, 10-500 M_☉, Yoon et al. (2012), rotation vk=0.4: [v1.1] (32 Mb)
Pop III tracks, 10-100 M_☉, Windhorst al. (2018): [v1.0] (5 Mb)
Pop III tracks, 9-120 M_☉, Murphy et al. (2021), no rotation: [v1.0] (29 Mb)
Pop III tracks, 1.7-120 M_☉, Murphy et al. (2021), with and without rotation: [v1.1] (131 Mb)
Pop III tracks, 100-1000 M_☉, Volpato et al. (2023): [v1.0] (6 Mb)
Pop III tracks, 6-2000 M_☉, Costa et al. (2025), including pre-main sequence evolution: [v1.1] (247 Mb)

Note: v1.1 are models used in Wasserman et al. (2025).

These zipped archives contain AB magnitudes in a selection of JWST (NIRCam and MIRI) and HST filters for stars at the same selection ages for which spectra are available. Magnitudes have been computed at redshifts z=1-20, in redshifts increments of 1.0, but please don't be shy to reach out if you need higher redshift resolution, redshifts outside this range or predictions for different filters. All magnitudes are computed under the assumption of an Ω_M=0.3, Ω_Λ=0.7, H₀=70 km s^-1 Mpc^-1 cosmology. At z≥5.8, all flux shortward of the Lyman-α limit is assumed to be absorbed by the neutral intergalactic medium. At lower redshifts, no absorption shortward of the Lyman-α limit is applied.

10% solar tracks, 9-575 M_☉, Szécsi et al. (2022): [v1.0 NIRCam], [v1.0 MIRI], [v1.0 HST]
Pop III tracks, 10-1000 M_☉, Yoon et al. (2012): [v1.0 NIRCam], [v1.0 MIRI], [v1.0 HST]
Pop III tracks, 10-100 M_☉, Windhorst al. (2018):[v1.0 NIRCam], [v1.0 MIRI], [v1.0 HST]
Pop III tracks, 9-120 M_☉, Murphy et al. (2021): [v1.0 NIRCam], [v1.0 MIRI], [v1.0 HST]
Pop III tracks, 100-1000 M_☉, Volpato et al. (2023): [v1.0 NIRCam], [v1.0 MIRI], [v1.0 HST]

These zipped archives contain rest-frame H-, He- and He⁺-ionzing fluxes plus Lyman-Werner fluxes for stars at various ages.

10% solar tracks, 9-575 M_☉, Szécsi et al. (2022): [v1.0]
Pop III tracks, 10-1000 M_☉, Yoon et al. (2012): [v1.0] [v1.1]
Pop III tracks, 10-100 M_☉, Windhorst al. (2018): [v1.0] [v1.1]
Pop III tracks, 9-120 M_☉, Murphy et al. (2021): [v1.0] [v1.1]
Pop III tracks, 100-1000 M_☉, Volpato et al. (2023): [v1.0] [v1.1]
Pop III tracks, 6-2000 M_☉, Costa et al. (2025): [v1.1]

Note: v1.1 are the models used in Wasserman et al. (2025). These feature a more accurate integration procedure (mainly affecting the HeII-ionizing flux) and supersedes the v.1.0 models. The v1.1 set also feature more models for rotating stars, plus models based on the Costa et al. (2025) stellar evolutionary tracks for Pop III stars.