Volume 607, November 2017
|Number of page(s)||12|
|Section||Numerical methods and codes|
|Published online||24 November 2017|
Ray-tracing 3D dust radiative transfer with DART-Ray: code upgrade and public release
1 University of Central Lancashire, Jeremiah Horrocks Institute, Preston, PR1 2HE, UK
2 The Astronomical Institute of the Romanian Academy, Str. Cutitul de Argint 5, Bucharest 052034, Romania
3 Max Planck Institute für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
4 The Carnegie Observatories – Carnegie Institution for Science, 813 Santa Barbara St, Pasadena, CA 91101, USA
Received: 10 August 2017
Accepted: 7 September 2017
We present an extensively updated version of the purely ray-tracing 3D dust radiation transfer code DART-Ray. The new version includes five major upgrades: 1) a series of optimizations for the ray-angular density and the scattered radiation source function; 2) the implementation of several data and task parallelizations using hybrid MPI+OpenMP schemes; 3) the inclusion of dust self-heating; 4) the ability to produce surface brightness maps for observers within the models in HEALPix format; 5) the possibility to set the expected numerical accuracy already at the start of the calculation. We tested the updated code with benchmark models where the dust self-heating is not negligible. Furthermore, we performed a study of the extent of the source influence volumes, using galaxy models, which are critical in determining the efficiency of the DART-Ray algorithm. The new code is publicly available, documented for both users and developers, and accompanied by several programmes to create input grids for different model geometries and to import the results of N-body and SPH simulations. These programmes can be easily adapted to different input geometries, and for different dust models or stellar emission libraries.
Key words: radiative transfer / scattering / methods: numerical / dust, extinction / infrared: ISM
© ESO, 2017
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