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Simple Stellar Population Datasets

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Andrew Benson edited this page Mar 8, 2022 · 13 revisions

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.

Bruzual & Charlot (2003)

Models from Bruzual & Charlot (2003; MNRAS; 344; 1000). Data was downloaded from http://www2.iap.fr/users/charlot/bc2003/.

  • 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;

BPASS

v2.0.0

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 http://flexiblelearning.auckland.ac.nz/bpass/2/files/.

  • 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

v2.2.1

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.

  • 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

Conroy et al. (2010)

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

  • SSP_Spectra_Conroy-et-al_v2.5_imfChabrier.hdf5
  • SSP_Spectra_Conroy-et-al_v2.5_imfKroupa.hdf5
  • SSP_Spectra_Conroy-et-al_v2.5_imfSalpeter.hdf5

Maraston

Models from Maraston (2005, MNRAS, 362, 799); Maraston (1998, MNRAS, 300, 872). Data downloaded from http://www-astro.physics.ox.ac.uk/~maraston/Claudia%27s_Stellar_Population_Models.html.

  • SSP_Spectra_Maraston_hbMorphologyRed_imfKroupa.hdf5
  • SSP_Spectra_Maraston_hbMorphologyRed_imfSalpeter.hdf5
  • SSP_Spectra_Maraston_hbMorphologyBlue_imfKroupa.hdf5
  • SSP_Spectra_Maraston_hbMorphologyBlue_imfSalpeter.hdf5

Venkatesan

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

  • SSP_Spectra_Venkatesan_PopIII_m10:140.hdf5
  • SSP_Spectra_Venkatesan_PopIII_m1:100.hdf5
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