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.
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.
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.
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.
