6/13/2023 0 Comments Boinc projekt![]() ![]() With the pixel SED fitting output we also hope to constrain parametric models of galaxy morphology in a more meaningful way than ordinarily achieved. ![]() Studies are underway investigating the potential biases that are introduced into results from integrated (total) SED fitting versus the pixel-by-pixel approach. We are starting to work on science outcomes (Thilker et al., in prep.). Table 1: The BOINC tasks developed for theSkyNet POGS. Move the HDF5 file to long term high availability storage. Once all the pixels for are galaxy are completed generate the HDF5 file.Ĭheck to see if all the pixels for a galaxy are completed. Once a galaxy has been archived after N days delete the database entries. If it has fallen below a threshold generate more work units.Įnsure the users are credited for the areas of a galaxy they worked on.īuild the PNG images that show the latest μ, M ∗, L t o t d and ψ ( t ) maps. Table 1 shows the major tasks that we developed to enable the smooth running of the system with minimal operator intervention. We use this for generating new work units and collating the data once all the pixels of a galaxy are complete. The BOINC middleware comes with a simple task scheduling system. In particular, we will fit multi-component (bulge, bar, disk) trial galaxy models, directly to the distribution of stellar mass rather than surface brightness in a single band, which is locally biased by star formation activity and dust obscuration. With the resultant pixel SED fitting output, we will then constrain parametric models of galaxy morphology in a more meaningful way than ordinarily achieved. This will provide us with physical parameters about the galaxy, such as: the stellar mass, star formation rate (SFR), dust attenuation, and first-order star formation history (SFH). We believe this can be done in 2-3 years with theSkyNet using the BOINC middleware (BOINC, 2013a).įor each catalogued galaxy meeting our selection criteria, the computers of our volunteers are being harnessed, via the Internet, to perform pixel-by-pixel spectral energy distribution (SED) fitting. This large volume of data would take many tens of years to process on a large University computing cluster. TheSkyNet Pan-STARRS1 Optical Galaxy Survey (POGS) project (POGS, 2013) was created to efficiently process and interpret the multi-wavelength data from the resolved galaxies detected by PS1.
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