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BPASS version 2.0

BPASS version 2.0 is now deprecated. Version 2.1 will be released in October 2017

These are the new version of BPASS results. The following have been improved and included:

  • There are now 10 times more stellar binary models than before, approximately 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 a future paper (Eldridge et al, in prep).

Each file below is for a different IMF (as described) and provides data for metallicities of Z=0.001, 0.002, 0.003, 0.004, 0.006, 0.008, 0.010, 0.014, 0.020, 0.030 and 0.040. The files include results for single-stars and binaries (labelled as 'bin' in output files). Solar Metallicity is in the range 0.014-0.020. They present the results for an instanteous starburst with a total mass of 1e6 Msun, (subdirectories OUTPUT_POP) as well as results for continuous star-formation at a rate of 1Msun/yr (such that the stellar mass is equal to the age of the population, subdirectories OUTPUT_CONT). Note the time bins are logarithmic so must be treated with care when combining the models to reproduce different star-formation histories. We will release codes shortly that demonstrate how to do this as well as create inputs for photoionization codes such as Cloudy and MAPPINGS (see Emission Lines page). Data are stored on Google Drive as tar files, each of which unpack into a directory structure labelled by IMF.

The links in BOLD are our fiducial models (two Salpeter-like IMFs, with diffferent upper mass limits).


SEDs

These files contain the primary output which is the stellar spectral energy distribution. Each file is for a different IMF as described. In addition each file contains two directories "OUTPUT_CONT" and "OUTPUT_POP"; these contain the continous and instanteous star-formation histories respectively.

Each file has 42 columns and 100000 rows. The first column is the wavelength of the SED and each subsequent n-th column holds the flux at the given wavelength for the stellar population at an age of 10^(6+0.1*(n-2)) years. The units of flux are Solar Luminosities per Angstrom for either a single aged cluster with total mass 1e6 Msun or a population with 1 Msun/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

Models are as described above.

Each file has 5 columns and 41 rows. The first column of the n-th row contains the age (spaced at intervals of 10^(6+0.1*(n-1)) years) for that row of numbers. The second column has the numbers of ionizing photons generated per second, 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. All these quantites are presented as log10(Flux).

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

Models are as described above.

Each file has 14 columns and 41 rows. The first column of the n-th row contains the age (in intervals of 10^(6+0.1*(n-1)) years) for that row of numbers. The remaining columns hold the absolute Vega magnitudes for the integrated stellar population at that redshift. From the 2nd to the 19th column these are UBVRIJHKugris. 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. However note that these are for the stellar emission only.

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

Models are as described above.

Each file has 21 columns and 41 rows. The first column of the n-th row contains the age (in intervals of 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 for O, Of, B, A, YSG, K, M, WNH, WN & WC stars respecitvely. Note for models with Z=0.004 and below the WNH population is incorrect; they include stars that would not be observed as WR stars as they are still core-hydrogen burning, but which move into a region of the HR diagram where our simple indentification routine counts 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 and tabulate. If you want them please email, they'll be released once a more detailed instruction manual has been released.

CORE-COLLAPSE SUPERNOVA RATES

Models as described above

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. Note that we do not calculate type 1a rates in this 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


Binary Stellar Models - v2.0

These are binary stellar evolution 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