"As we discover , we suffer from a variety of s, both in our nearby and distant searches. The most significant effect is – a selection effect which leads brightness limited searches finding brighter than average objects near their sensitivity limit. This bias is caused by the larger volume in which bright objects can be uncovered compared to their fainter counterparts. Malmquist bias errors are proportional to the square of the intrinsic dispersion of the distance method, and because SN Ia are such accurate distance indicators, these errors are quite small – approximately 2%. We use s to estimate these effects, and remove their effects from our s."
Brian Paul Schmidt is an American Australian astrophysicist at the Australian National University's Mount Stromlo Observatory and Research School of Astronomy and Astrophysics. He was the Vice-Chancellor of the Australian National University (ANU) from January 2016 to January 2024. He is known for his research in using supernovae as cosmological probes. He previously held a Federation Fellowship a
"… one does not expect a . To my mind, I was genuinely surprised because when you make a discovery of acceleration–well, what causes the acceleration? Well, we give it a name––but we don’t understand it yet. I would not be surprised if we don’t understand it during my lifetime. Without understanding it, I felt it wouldn’t be worthy of a Nobel Prize. The fact that it was given pretty timely–you know, I was only 44 last year–was a bit of surprise."
Brian Schmidt"With the as an anchor, theory converged on a standard model of the universe, which was still in place in 1998, at the time of our discovery of the . This standard model was based on the theory of general relativity, and two assumptions. assumption one was that the , and assumption two that it is composed of normal , i.e. matter whose density falls directly in proportion to the volume of space, which it occupies. Within this framework, it was possible to devise observational tests of the overall theory, as well as provide values for the fundamental constants within this model – the current expansion rate (), and the average density of matter in the universe. For this model, it was also possible to directly relate the density of the universe to the rate of cosmic deceleration and the geometry of space. it stated that the more material the faster the deceleration, that above a critical density the universe has a and below this a ."
Brian Schmidt