I study type Ia supernovae. With good measurements, these supernovae can be used as “standard candles,” meaning their apparent brightness gives their distances. These distances help us measure the expansion history of the universe while the objects themselves are astrophysically important.

Using these supernovae for cosmology requires many careful steps, from the search, to detailed pixel-level models of the images for accurate photometry (brightness measurements), to statistical techniques for the accurate estimation of uncertainties.

The Search for SNe

  • Combining ground and space telescopes—Subaru and Hubble—we can collect the largest sample of high-redshift SNe (z>1) in a single survey. The SUbaru Supernovae with Hubble Infrared (SUSHI) HST program (co-PI’d with Nao Suzuki) is currently collecting IR data on these high-redshift SNe discovered in the Subaru Strategic Program. Read more about the SUSHI program.
  • The next generation of space-based observing will rely on two telescopes, James Webb (under construction) and WFIRST (planned). I am currently calculating the specifications of WFIRST for optimal supernova cosmology. Read more about my work on WFIRST.

Modeling the Images

Statistical Techniques and other Computation Considerations 

  • Current cosmological analyses are limited by their inability to properly model outliers, selection effects, shape- and color-standardization relations, unexplained dispersion, and heterogeneous observations… until UNITY. Using Bayesian Hierarchical modeling, my framework, the Unified Nonlinear Inference for Type-Ia cosmologY (UNITY), simultaneously models each of these factors and significantly reduces our statistical and systematic uncertainties. Read more about my work on UNITY.
  • When possible, I perform my studies using “blinded analyses,” which help protect researchers from inadvertently tweaking their analysis steps until they obtain their expected results.