Latest BPASS v2.0 RESULTS 

These are the new version of BPASS results. The following has been 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.

 

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 instrcution 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