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Previous older BPASS versions


BPASSv1

Stellar Models - v1.0

Single star stellar tracks with UBVRIJHK broad-band colours.

Metallicities of Z=0.001, 0.004, 0.008, 0.020, 0.040 with masses from 0.1 to 120M(Sun).

[ DOWNLOAD GZIPPED TARBALL]

 

Sample Binary Stellar Models - v1.0

These are sample binary tracks (11 models from 15,000!) giving the details of the primary star only, for one separation and a mass ratio of 0.5. More models will be available when a suitable distribution system is created.

[ DOWNLOAD GZIPPED TARBALL]

Solar metallicity (Z=0.020) binary models for all stars that end hydrogen free, i.e. "Wolf-Rayet" stars. File format is the same as for above files.

[DOWNLOAD GZIPPED TARBALL]

 

Stellar Populations Broad-band colours - v1.1

Magnitudes in various filters for both single and binary star populations with a canonical IMF.

Both constant star-formation and an instanteous bursts at ages from 1Myr to 10Gyr. Metallicities of Z=0.001, 0.004, 0.008, 0.020, 0.040

Filters given are UBVRIJHK and equivalent HST filters.

[ DOWNLOAD GZIPPED TARBALL]

 

Stellar Populations SEDs - v1.1

Full spectral energy distributions including stellar & nebular components from 30 to 30000A for both single and binary star populations with a canonical IMF.

Both constant star-formation and an instanteous bursts at ages from 1Myr to 10Gyr. Metallicities of Z=0.001, 0.004, 0.008, 0.020, 0.040

[ DOWNLOAD GZIPPED TARBALL FOR Z=0.001]

[ DOWNLOAD GZIPPED TARBALL FOR Z=0.004]

[ DOWNLOAD GZIPPED TARBALL FOR Z=0.008]

[ DOWNLOAD GZIPPED TARBALL FOR Z=0.020]

[ DOWNLOAD GZIPPED TARBALL FOR Z=0.040]

 

Nebula Emission Line Fluxes - v1.1

Nebula emission line fluxes versus age for different metallicities and single/binary populations, calculated by Cloudy.

[ DOWNLOAD GZIPPED TARBALL]

 

Stellar Emission Line Fluxes - v1.1

Stellar emission line fluxes versus age for different metallicities and single/binary populations, calculated from the models. Included as equivalent widths and line luminosities for C(IV), He(II) and the Wolf-Rayet Blue & Red bumps.

[ DOWNLOAD GZIPPED TARBALL]

 

Sample Binary Stellar Stellar Population Number Ratios - v1.0

 Results from Eldridge, Izzard & Tout (2008) Population synthesis v1.0:

 

 

WR/O

WR/O

BSG/RSG

BSG/RSG

RSG/WR

RSG/WR 

WC/WN

WC/WN

Ibc SNe

/ II SNe

Ibc SNe

 

/ II SNe

 

Z

[O/H]      

Sin

Bin

Sin

Bin

Sin

Bin

Sin

Bin

Sin

Bin

0.001

7.5 +/-0.1

0.001

0.012

14.7

46.5

18.9

0.28

0.070 

0.012

0.003 

0.023

0.004

8.1 +/-0.1

0.0085

0.024

3.47 

13.1

11.9

0.86

0.15

0.098 

0.018  

0.098

0.008

8.4 +/-0.1

0.012

0.031

3.22 

13.8

11.3

0.78 

0.43

0.20  

0.036

0.25 

0.020

8.8 +/-0.2

0.026

0.051

3.73

15.6 

6.78  

0.68

0.97 

0.42

0.054 

0.43

0.040

9.0 +/-0.2

0.059

0.090

4.86 

18.2

3.21

0.48

1.04

0.49

0.054

0.49

                              

 

 

 

 

BPASSv2.0

BPASS v2.0 RESULTS 

These were the first release version after the major update to BPASS. The following was improved and included:

  • There are now 10 times more stellar binary models than before, approximatel 150,000.
  • The treatment of the secondary stars is now improved with more remnant masses included.
  • The spectral synthesis code has been rewritten to be faster and more consistent.
  • There are now more data outputs included in the release files.
  • We have included all of the new PoWR atmosphere models for Wolf-Rayet stars.
  • Interacting binary stars are now included in all models from 0.1 to 300 MSun.
  • An initial period distribution for the binary parameters is now used rather than an initial separation distribution. The one employed is similar to that inferred from observations.

These have been calculated by the NeSI Pan Cluster. If you use these results please acknowledge BPASS and NeSI, these will be described in detail in future papers. 

Each file below covers all metallcities from Z=0.001, 0.002, 0.003, 0.004, 0.006, 0.008, 0.010, 0.014, 0.020, 0.030 and 0.040 and the files include those for single-stars and binaries. They also include the results for an instanteous starburst with a total mass of 1e6 Msun as well as results for continuous star-formation of 1Msun/yr. Note the time bins are logarithmic so must be treated with care when combining the models with various star-formation histories. We will release codes shortly that demonstrate how to do this as well as create inputs for photoionization codes of Cloudy and MAPPINGS.

The links in BOLD are out fiducial models.

Please note there are some known issues in this release which will be fixed in the version released when the instrument paper is submitted. These issues are as follow:

  • I-band fluxes are wrong by about a magnitude.
  • Some of the SED files include negative values, these should be set to zero.
  • If you require constant star-formation history values we suggest that you use the OUTPUT_POP values rather than those provided for OUTPUT_CONT for the supernova rates.

Please contact us if you find further issues.

The files can be accessed either by using the links below of my browsing the Google Drive directly using this link: 

https://drive.google.com/open?id=0B7vqPPPgOdtIfjUtb3RsV2JUOTFFX29WV1FZNURPMHAxTEtZQjhJOGtyNXZUTTNVSzFZazQ

 

SEDs

These files contain the primary output which is the stellar spectral energy distribution. Each file is for the IMF given on the link. In addition each file contains two directories "OUTPUT_CONT" and "OUTPUT_POP" that contains the continous and instanteous star-formation histories. 

Each file has 42 columns and 100000 rows. The first column is the wavelength of the SED and each subsequent n-th column has the flux for the population at an age of 10^(6+0.1*(n-2)) years. Each row than the flux at the wavelength given in the first column, the units of flux are Solar Luminosities per Angstrom for either a cluster of 1e6Msun or 1Msun/yr of star-formation.

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 100Msun

IMF slope of -2.35 from 0.1 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 300Msun

 IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 100Msun

 
IONIZING FLUX PREDICTIONS

These files contain the primary output which is the stellar spectral energy distribution. Each file is for the IMF given on the link. In addition each file contains two directories "OUTPUT_CONT" and "OUTPUT_POP" that contains the continous and instanteous star-formation histories. 

Each file has 5 columns and 41 rows. The first column of the n-th row contains the age 10^(6+0.1*(n-1)) years for that row of numbers. The second column has the numbers of ionizing photons, the second an estimate of the H-alpha flux in erg/s, the third and fourth rows have the FUV and NUV flux in erg/s/A. The values are for either a cluster of 1e6Msun or 1Msun/yr of star-formation.

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 100Msun

IMF slope of -2.35 from 0.1 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 100Msun

BROAD-BAND COLOURS - UBVRIJHKugriz

These files contain the primary output which is the stellar spectral energy distribution. Each file is for the IMF given on the link. In addition each file contains two directories "OUTPUT_CONT" and "OUTPUT_POP" that contains the continous and instanteous star-formation histories. 

Each file has 14 columns and 41 rows. The first column of the n-th row contains the age 10^(6+0.1*(n-1)) years for that row of numbers. The remaining columns hold the absolute Vega magnitudes for the stellar populations. The 2nd column is V-I while the 3rd to the 15th column these are UBVRIJHKugriz. The values are for either a cluster of 1e6Msun or 1Msun/yr of star-formation.The files with "ha" in their filename include the H-alpha flux contribution to the R-bands.

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 100Msun

IMF slope of -2.35 from 0.1 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 100Msun

 
RESOLVED STELLAR POPULATION NUMBER COUNTS

These files contain the primary output which is the stellar spectral energy distribution. Each file is for the IMF given on the link. In addition each file contains two directories "OUTPUT_CONT" and "OUTPUT_POP" that contains the continous and instanteous star-formation histories. 

Each file has 21 columns and 41 rows. The first column of the n-th row contains the age 10^(6+0.1*(n-1)) years for that row of numbers. The remaining columns hold the number of stars of different types split into two luminosity classes. Columns 2 to 11 have luminosities with log(L/Lsun) > 4.9, columns 12-21 have luminosities below this limit. Columns 2-11/12-21 are O, Of, B, A, YSG, K, M, WNH, WN & WC. Respecitvely. Note for models with Z=0.004 and below the WNH population is incorrect as they include stars that would not be observed as WR stars as they are still core-hydrogen burning but move into a region of the HR diagram where our simple indentification routine makes them as WR stars. This will be altered in a future release.

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 100Msun

IMF slope of -2.35 from 0.1 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 100Msun

 
Hertzsprung-Russell DIAGRAM ISOCONTOURS
These are complex to explain. If you want them please email, they'll be released once a more detailed instruction manual has been released.

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 100Msun

IMF slope of -2.35 from 0.1 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 300Msun

 IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 100Msun

 
SUPERNOVA RATES

These files contain the primary output which is the stellar spectral energy distribution. Each file is for the IMF given on the link. In addition each file contains two directories "OUTPUT_CONT" and "OUTPUT_POP" that contains the continous and instanteous star-formation histories. 

Each file has 6 columns and 41 rows. The first column of the n-th row contains the age 10^(6+0.1*(n-1)) years for that row of numbers. The remaining columns hold the number (not rate) of supernovae of different types, columns 2-6 are respectively types IIP, non-IIP, blank, Ib and Ic.

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.00 from 0.5 to 100Msun

IMF slope of -2.35 from 0.1 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 300Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.35 from 0.5 to 100Msun

IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 300Msun

 IMF slopes of -1.30 between 0.1 to 0.5Msun and -2.70 from 0.5 to 100Msun

 

Binary Stellar Models - v2.0

These are binary tracks, 5565 per metallicity from the latest version of BPASS. These are only for the evolution of the primary star. They are for a range of initial masses from 0.1 to 300 Msun, mass ratios 0.1, 0.3, 0.5, 0.7 and 0.9, and initial periods from 1 day 10000 days

Each file is a gzipped tar file. For the structure of the filenames and columns in each file please read this readme file.

Be aware these files are large and we suggest using one metallicity to explore the models before you download them all.

Also we have not had time to check all these files so please contact us if you find something odd or have questions.

Z=0.001  https://drive.google.com/file/d/0B7vqPPPgOdtIS0NOOEptZHpIVDA/view?usp=sharing
Z=0.002  https://drive.google.com/file/d/0B7vqPPPgOdtITTBWTUVFME04aGc/view?usp=sharing
Z=0.003  https://drive.google.com/file/d/0B7vqPPPgOdtIb3ZHWS1IVzllRkU/view?usp=sharing
Z=0.004  https://drive.google.com/file/d/0B7vqPPPgOdtIZ0V6RnR6aWhwREU/view?usp=sharing
Z=0.006  https://drive.google.com/file/d/0B7vqPPPgOdtIME9KNF9Xa1FHdXc/view?usp=sharing
Z=0.008  https://drive.google.com/file/d/0B7vqPPPgOdtIMU4yNzBpSk43Wjg/view?usp=sharing
Z=0.010  https://drive.google.com/file/d/0B7vqPPPgOdtIR0JmVV9CNzJlSWM/view?usp=sharing
Z=0.014  https://drive.google.com/file/d/0B7vqPPPgOdtIc0hhNGNMaldJdnc/view?usp=sharing
Z=0.020  https://drive.google.com/file/d/0B7vqPPPgOdtIVTB4STc5ZFVBdkU/view?usp=sharing
Z=0.030  https://drive.google.com/file/d/0B7vqPPPgOdtIaFJ2bDlUZ21LUUE/view?usp=sharing
Z=0.040  https://drive.google.com/file/d/0B7vqPPPgOdtIa2dBOGVVTE9mTlk/view?usp=sharing
 

 

Nebula Emission Line Fluxes - v2.0

BPASS produces stellar continuum emission. We caution that, in astrophysical contexts, this is reprocessed by dust and nebular gas before detection, and that our models should be similarly processed.

We recommend the use of a radiative transfer code such as CLOUDY or MAPPINGS to do this.

We have been wary of providing a processed data set, since there is considerable uncertainty on the physical range of nebular gas parameters and it is important to distinguish between uncertainties in the stellar models and those in their later reprocessing.

In published work (e.g. Stanway et al 2014) and our earlier work on BPASS v1.1 (below) we have used CLOUDY v13.03 and defined a default set of nebular gas parameters as follows:

  • gas metallicity follows stellar metallicity,
  • log(electron density)=2,
  • covering fraction=1,
  • spherical geometry, inner radius=10 pc.

Input files for CLOUDY with these parameters can be generated in IDL using this code. The code can be modified for other gas properties as required.

 
 
 
 
 

BPASSv2.1

Latest BPASS version 2.1 Data Release (October 2017)

This version of BPASS represents an extension and modification of our older v1 and v2.0 models.

The more important new features and results included in this release of BPASS include: calculation of a significantly larger number of stellar models, release of a wider variety of predictions of stellar populations, inclusion of new stellar atmosphere models, a wider range of metallicities, binary models are now included for the full stellar mass range and a broader range of compact remnant masses are now calculated in secondary models.

Most crucially, BPASS has now been fully described in a peer-reviewed paper: Eldridge, Stanway et al, 2017, PASA in press.

We have also produced a User Manual which we strongly recommend users examine. This is available typeset in both Arial and OpenDyslexic (a font designed for use by those with specific learning differences).

The data release is routinely stored on Google Drive at

https://drive.google.com/drive/folders/0B7vqPPPgOdtIdjdyV3JwODZ3TlU,

and will be available soon from the PASA data store. We caution that the full data release is very large (particularly if individual stellar models are downloaded). It comprises a directory structure, sorted by IMF, with tarballs containing data products as follows:

1. Stellar Model Outputs:

  • Binary stellar models with photometric colours
  • New OB stars atmosphere models

2. Stellar Population Outputs (all versus age):

  • Massive star type number counts
  • Core collapse supernova rates
  • Yields, energy output from winds and supernovae and ejected yields of X , Y and Z
  • Stellar population mass remaining
  • HR diagram (isochronal contours)

3. Spectral Synthesis Outputs (all versus age):

  • Spectral Energy Distributions
  • Ionizing flux predictions
  • Broadband colours
  • Colour-Magnitude Diagram (CMD) making code

For full details, and README details for the data files, we again recommend the User Manual.

We would appreciate the inclusion of the following acknowledgement where appropriate:
“This work made use of v2.1 of the Binary Population and Spectral Synthesis (BPASS) models as last described in Eldridge, Stanway et al (2017).”

 

License: The results from BPASS and CURVEPOPS available on this site licensed under a Creative Commons Attribution-NonCommercial 4.0 International License.

Creative Commons License
 

 
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