High redshift observations of Type Ia Supernovae (SN) provided the first convincing evidence for the existence of Dark Energy (DE). These observations remain one of the most useful tools for constraining cosmological parameters. Despite numerous advances in observational and theoretical techniques towards understanding Type Ia SN, there remain many potential systematic uncertainties that can limit the cosmological precision obtainable from SN surveys. These systematic uncertainties have become the limiting factor in SN constraints on DE. It is the goal of the Supernova Hub to carry out a research program to understand and reduce these potential systematic errors, thereby improving SN as cosmological probes.

The SDSS survey telescope stands out against the breaktaking backdrop of the Sacramento Mountains.
The Supernova Hub will carry out a program to improve supernovae as cosmological distance indicators by reducing the major systematic errors, and evaluating more subtle uncertainties that have been essentially ignored in previous works. In the process, the SN Hub will extract the most precise and reliable cosmological results from recent and on-going SN surveys, and lay the groundwork for future surveys to achieve stronger constraints on the nature of dark energy. The hub will analyze SN light curves from a joint collaboration between the SDSS-II Supernova Survey and the Supernova Legacy Survey (SNLS). The resulting data set and analysis tools will be used for the upcoming Dark Energy Survey and to prepare the SN program for the Large Synoptic Survey Telescope (LSST).

The Type Ia supernova research team is using the FLASH computer code to conduct the first comprehensive, systematic validation of all current SN Ia models.
The data will also be used to compare to detailed 3-dimensional Type Ia SN simulations produced by the University of Chicago Alliances Center for Astrophysical Thermonuclear Flashes and their suite of numerical codes. By providing a comprehensive dataset and analysis code for comparison, theoretical models will be evaluated much more rigorously than in previous efforts, leading to a better understanding of the Type Ia explosion mechanism. The ultimate goal is that FLASH simulations provide useful feedback into SN-cosmology analyses by constraining or characterizing SNIa properties such as the nature of color variations or why the brightness depends slightly on the host-galaxy mass.