Cosmological Constraints from Measurements of Type Ia Supernovae Discovered during the First 1.5 yr of the Pan-STARRS1 Survey
Price, P. A.; Berger, E.; Challis, P.; Kirshner, R. P.; Rest, A.; Foley, R. J.; Wood-Vasey, W. M.; Smartt, S. J.; Chambers, K. C.; Stubbs, C. W.; Denneau, L.; Huber, M. E.; Flewelling, H.; Magnier, E. A.; Waters, C.; Wainscoat, R.; Kotak, R.; Chornock, R.; Riess, A.; Lunnan, R.; Tonry, J. L.; Rodney, S.; Smith, K.; Botticella, M. T.; Brout, D.; Scolnic, D.; Metcalfe, N.; Burgett, W. S.; Kaiser, N.; Valenti, S.; Soderberg, A. M.; Draper, P. W.; Hodapp, K. W.; Zheng, Z.; Schlafly, E.; Thilker, D.; Sanders, N. E.; Milisavljevic, D.; Marion, G. H.; Czekala, I.; Drout, M.; Hudson, M. J.; Narayan, G.; Kudritzki, R. -P.; Pastorello, A.; Leibler, C.; McCrum, M.; Stafford, E.; Sweeney, W.
United States, United Kingdom, Germany, Italy, Canada
Abstract
We present griz P1 light curves of 146 spectroscopically confirmed Type Ia supernovae (SNe Ia 0.03 < z < 0.65) discovered during the first 1.5 yr of the Pan-STARRS1 Medium Deep Survey. The Pan-STARRS1 natural photometric system is determined by a combination of on-site measurements of the instrument response function and observations of spectrophotometric standard stars. We find that the systematic uncertainties in the photometric system are currently 1.2% without accounting for the uncertainty in the Hubble Space Telescope Calspec definition of the AB system. A Hubble diagram is constructed with a subset of 113 out of 146 SNe Ia that pass our light curve quality cuts. The cosmological fit to 310 SNe Ia (113 PS1 SNe Ia + 222 light curves from 197 low-z SNe Ia), using only supernovae (SNe) and assuming a constant dark energy equation of state and flatness, yields w=-1.120+0.360-0.206{(Stat)} +0.269-0.291{(Sys)}. When combined with BAO+CMB(Planck)+H 0, the analysis yields Ω _M=0.280+0.013-0.012 and w=-1.166+0.072-0.069 including all identified systematics. The value of w is inconsistent with the cosmological constant value of -1 at the 2.3σ level. Tension endures after removing either the baryon acoustic oscillation (BAO) or the H 0 constraint, though it is strongest when including the H 0 constraint. If we include WMAP9 cosmic microwave background (CMB) constraints instead of those from Planck, we find w=-1.124+0.083-0.065, which diminishes the discord to <2σ. We cannot conclude whether the tension with flat ΛCDM is a feature of dark energy, new physics, or a combination of chance and systematic errors. The full Pan-STARRS1 SN sample with ~three times as many SNe should provide more conclusive results.