Simple Stellar Population Datasets - galacticusorg/galacticus GitHub Wiki

This pages provides links to several datasets containing tabulations of stellar population spectra as a function of age and metallicity. All files are in the prefered format used by Galacticus, and have been derived from a variety of published sources.

Models from Bruzual & Charlot (2003; MNRAS; 344; 1000). Data was downloaded from http://www.bruzual.org/bc03/Original_version_2003/.

Download from Zenodo

• SSP_Spectra_BC2003_lowResolution_imfChabrier.hdf5: Low-resolution, Chabrier IMF;
• SSP_Spectra_BC2003_lowResolution_imfSalpeter.hdf5: Low-resolution, Salpeter IMF;
• SSP_Spectra_BC2003_highResolution_imfChabrier.hdf5: High-resolution, Chabrier IMF;
• SSP_Spectra_BC2003_highResolution_imfSalpeter.hdf5: High-resolution, Salpeter IMF;

The BPASS models of Eldridge & Stanway (2012, MNRAS, 419, 479); Eldridge, Langer & Tout (2011, MNRAS, 414, 3501); Eldridge & Stanway (2009, MNRAS, 400, 1019); Eldridge, Izzard & Tout (2008, MNRAS, 384, 1109). Data was downloaded from the now defunct Google drive link https://drive.google.com/open?id=0B7vqPPPgOdtIfjUtb3RsV2JUOTFFX29WV1FZNURPMHAxTEtZQjhJOGtyNXZUTTNVSzFZazQ.

Download from Zenodo

• SSP_Spectra_BPASS_binary.hdf5
  • Canonical BPASS IMF
  • Includes binary stars
  • Uses v2.0 of BPASS
• SSP_Spectra_BPASS_single.hdf5
  • Canonical BPASS IMF
  • Does not include binary stars
  • Use v2.0 of BPASS

The BPASS models of Eldridge, Stanway et al. (2017) and Stanway & Eldridge et al. (2018). Data was downloaded from https://drive.google.com/drive/folders/1BS2w9hpdaJeul6-YtZum--F4gxWIPYXl?usp=sharing.

Download from Zenodo

• SSP_Spectra_BPASSv2.2.1_bin-imf100_100.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.00 from 0.5M_☉ to 100M_☉)
  • Includes binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_bin-imf100_300.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.00 from 0.5M_☉ to 300M_☉)
  • Includes binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_bin-imf135_100.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 100M_☉)
  • Includes binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_bin-imf135_300.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Includes binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_bin-imf135all_100.hdf5
  • Power law IMF (α=-2.35 from 0.1M_☉ to 100M_☉)
  • Includes binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_bin-imf170_100.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.70 from 0.5M_☉ to 100M_☉)
  • Includes binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_bin-imf170_300.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.70 from 0.5M_☉ to 300M_☉)
  • Includes binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_bin-imf_chab100.hdf5
  • Chabrier IMF (α=-2.00; maximum mass 100M_☉)
  • Includes binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_bin-imf_chab300.hdf5
  • Chabrier IMF (α=-2.00; maximum mass 300M_☉)
  • Includes binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_sin-imf100_100.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.00 from 0.5M_☉ to 100M_☉)
  • Does not include binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_sin-imf100_300.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.00 from 0.5M_☉ to 300M_☉)
  • Does not include binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_sin-imf135_100.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 100M_☉)
  • Does not include binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_sin-imf135_300.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Does not include binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_sin-imf135all_100.hdf5
  • Power law IMF (α=-2.35 from 0.1M_☉ to 100M_☉)
  • Does not include binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_sin-imf170_100.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.70 from 0.5M_☉ to 100M_☉)
  • Does not include binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_sin-imf170_300.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.70 from 0.5M_☉ to 300M_☉)
  • Does not include binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_sin-imf_chab100.hdf5
  • Chabrier IMF (α=-2.00; maximum mass 100M_☉)
  • Does not include binary stars
  • Uses v2.2.1 of BPASS
• SSP_Spectra_BPASSv2.2.1_sin-imf_chab300.hdf5
  • Chabrier IMF (α=-2.00; maximum mass 300M_☉)
  • Does not include binary stars
  • Uses v2.2.1 of BPASS

The BPASS models of Eldridge, Stanway et al. (2017), Stanway & Eldridge et al. (2018) and Byrne et al. (2022, MNRAS in press). Data was downloaded from here.

Download from Zenodo

• SSP_Spectra_BPASSv2.3_sin-imf135_300-alpha-02.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Does not include binary stars
  • α-alement enhancement of Δlog₁₀(α/Fe)=-0.2
  • Uses v2.3 of BPASS
• SSP_Spectra_BPASSv2.3_sin-imf135_300-alpha+00.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Does not include binary stars
  • α-alement enhancement of Δlog₁₀(α/Fe)=+0.0
  • Uses v2.3 of BPASS
• SSP_Spectra_BPASSv2.3_sin-imf135_300-alpha+02.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Does not include binary stars
  • α-alement enhancement of Δlog₁₀(α/Fe)=+0.2
  • Uses v2.3 of BPASS
• SSP_Spectra_BPASSv2.3_sin-imf135_300-alpha+04.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Does not include binary stars
  • α-alement enhancement of Δlog₁₀(α/Fe)=+0.4
  • Uses v2.3 of BPASS
• SSP_Spectra_BPASSv2.3_sin-imf135_300-alpha+06.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Does not include binary stars
  • α-alement enhancement of Δlog₁₀(α/Fe)=+0.6
  • Uses v2.3 of BPASS
• SSP_Spectra_BPASSv2.3_bin-imf135_300-alpha-02.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Includes binary stars
  • α-alement enhancement of Δlog₁₀(α/Fe)=-0.2
  • Uses v2.3 of BPASS
• SSP_Spectra_BPASSv2.3_bin-imf135_300-alpha+00.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Includes binary stars
  • α-alement enhancement of Δlog₁₀(α/Fe)=+0.0
  • Uses v2.3 of BPASS
• SSP_Spectra_BPASSv2.3_bin-imf135_300-alpha+02.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Includes binary stars
  • α-alement enhancement of Δlog₁₀(α/Fe)=+0.2
  • Uses v2.3 of BPASS
• SSP_Spectra_BPASSv2.3_bin-imf135_300-alpha+04.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Includes binary stars
  • α-alement enhancement of Δlog₁₀(α/Fe)=+0.4
  • Uses v2.3 of BPASS
• SSP_Spectra_BPASSv2.3_bin-imf135_300-alpha+06.hdf5
  • Broken power law IMF (α=-1.30 from 0.1M_☉-0.5M_☉, α=-2.35 from 0.5M_☉ to 300M_☉)
  • Includes binary stars
  • α-alement enhancement of Δlog₁₀(α/Fe)=+0.6
  • Uses v2.3 of BPASS

Models from Conroy & Gunn (2010; ascl:1010.043).

Download from Zenodo

• SSP_Spectra_Conroy-et-al_v2.5_imfChabrier.hdf5
  • Computed with v2.5 of FSPS
  • Chabrier IMF
• SSP_Spectra_Conroy-et-al_v2.5_imfKroupa.hdf5
  • Computed with v2.5 of FSPS
  • Kroupa IMF
• SSP_Spectra_Conroy-et-al_v2.5_imfSalpeter.hdf5
  • Computed with v2.5 of FSPS
  • Salpeter IMF

Models from Maraston (2005, MNRAS, 362, 799); Maraston (1998, MNRAS, 300, 872). Data downloaded from http://www.icg.port.ac.uk/~maraston/Claudia's_Stellar_Population_Model.html.

Download from Zenodo

• SSP_Spectra_Maraston_hbMorphologyRed_imfKroupa.hdf5
  • Kroupa IMF
  • "Red" horizontal branch morphology
• SSP_Spectra_Maraston_hbMorphologyRed_imfSalpeter.hdf5
  • Salpeter IMF
  • "Red" horizontal branch morphology
• SSP_Spectra_Maraston_hbMorphologyBlue_imfKroupa.hdf5
  • Kroupa IMF
  • "Blue" horizontal branch morphology
• SSP_Spectra_Maraston_hbMorphologyBlue_imfSalpeter.hdf5
  • Salpeter IMF
  • "Blue" horizontal branch morphology

Models from Venkatesan et al. (2003; ApJ; 584; 621).

Download from Zenodo

• SSP_Spectra_Venkatesan_PopIII_m10:140.hdf5
  • Salpeter IMF from 10-140M_☉
• SSP_Spectra_Venkatesan_PopIII_m1:100.hdf5
  • Salpeter IMF from 1-100M_☉