DescriptionType Ia Supernovae (SNe Ia), the result of exploding carbon/oxygen white dwarfs, are powerful cosmological distance indicators. They are excellent standardizable candles, which must be corrected using parameters such as their lightcurve shape, color, or host galaxy properties. Properly standardizing SNe Ia is essential as there is currently a tension in the measurement of the Hubble constant, $H_0$, between local and early Universe measurements. In this thesis I will present work done with the Foundation Supernova Survey to investigate previously seen correlations between ejecta velocity and other supernova properties. Additionally, I will re-analyze previous results through the use of the lightcurve fitter SALT2 to create a uniform comparison. We find that while the previous results still show a clear offset in color between high-velocity and normal-velocity SNe, the Foundation data do not. Additionally, the Foundation data do not show a significant split in Hubble diagram residual either. Intriguingly, we find that SN Ia ejecta velocity information can possibly be determined from photometry, in the reddest bands, alone. For high-redshift SNe, these rest-frame wavelengths will be observed by the future Nancy Grace Roman Space Telescope. Our results are in line with work which suggests that SN Ia host-galaxy mass is correlated with ejecta velocity: high-velocity SNe Ia are nearly exclusively found in high-mass hosts. However, host-galaxy properties alone cannot clear the discrepancy between Foundation and the older data. Finally, I discuss the ongoing Hubble Space Telescope (HST) survey, Supernova in the Infrared avec Hubble (SIRAH). This low-redshift, infrared (IR) survey aims to create a legacy sample of high quality IR lightcurves and spectra to be used in future IR space and ground based surveys, most notably the Nancy Grace Roman Space Telescope which will observe thousands of SNe across a variety of redshifts and rest-frame bands. I present preliminary data from the SIRAH survey including two serendipitous observations. SN~2020bpi was the first object observed with SIRAH and was also observed by the Transiting Exoplanet Survey Satellite (TESS) which obtained extremely high cadence photometry of SN~2020bpi's explosion. Using this data, we can look for evidence of a companion star through excess flux. We have found no significant excess flux signature in SN~2020bpi, effectively putting an upper limit on the size of any possible companion. SN~2021hpr is a more recent SIRAH SN which exploded in the same galaxy as another SN already under observation. We were therefore able to obtain extremely early ($sim-18$ days) color information which is largely unprecedented in the field. I compare this early photometry to existing models of the similar SN~2018oh to attempt to draw conclusions as to the nature of its progenitor.