| |
 |
| Paper: |
Simulating Stellar Color-Magnitude Diagrams on the GPU |
| Volume: |
541, ADASS XXXIII |
| Page: |
249 |
| Authors: |
László Dobos; Carrie Filion; Tamás Budavári; Rosemary Wyse; Alexander S. Szalay |
| DOI: |
10.26624/KRRI6509 |
| Abstract: |
Generating synthetic photometric catalogs of fields containing a large
number of stars, that may belong to multiple stellar populations (such as the resolved
composite stellar populations of nearby satellite galaxies and the various sub populations of the Galactic foreground) is computationally intensive. Stellar populations are
usually characterized by their metallicity, age and distance distributions, which parameters are often correlated, whereas the initial mass of each star is thought to come from a
universal Initial Mass Function (IMF). Precomputed isochrone grids for a large number
of magnitude systems are available to convert these fundamental stellar parameters to
magnitudes. Interpolation between isochrones, however, must be done in the parameter called the Equivalent Evolutionary Phase (EEP), instead of initial mass, since stars
with the same initial mass - but slightly different age (or metallicity) - can be in entirely
different evolutionary phases. Hence, isochrone grids are tabulated for metallicity, age
and EEP and interpolation of magnitudes from metallicity, age and initial mass requires
an implicit interpolation scheme where one has to find the EEP as well, as part of the
solution. On the other hand, synthetic catalogs are often generated with given magnitude and color cuts which must be observed during random sampling. Due to the
steep IMF, the large number of low-mass, faint stars are likely to cause high random
sampling rejection rates. While intricate heuristics can help mitigate the latter problem,
our GPU-based solution to synthetic catalog generation is fast enough to generate hundreds of thousands of stars on the time scale of tens of seconds with broadly available
hardware. Our software library, built with eager mode TensorFlow, solves the implicit
isochrone interpolation problem, as well as provides a relatively simple, yet very flexible way of describing mixtures composite stellar populations for detailed modelling. |
|
|
|
|
|
