The characteristic density of an equilibrium halo is proportional to the density of the universe at the time it was assembled. Screen-use options. We describe a method for estimating the efficiency and purity of photometric SN Ia classification when spectroscopic confirmation of only a limited sample is available, and demonstrate that SN Ia candidates from SDSS-II can be identified photometrically with ~91% efficiency and with a contamination of ~6%. The supernova's light is just arriving at Earth because it has traveled more than 10 billion light-years (redshift 1.914) across space.The supernova, designated SN UDS10Wil, is nicknamed SN Wilson, after the 28th U.S. President, Woodrow Wilson. Both the mass-concentration and stellar-to-halo mass relations have significant scatter around the median relations.
R.P.K. While the spectral absorption features alone are unable to convincingly distinguish between a SN Ia and a SN Ib/c, SNe II have features that are inconsistent with the data (see Filippenko To classify SN UDS10Wil we compared the observed UDS10Wil light curve against Monte Carlo simulations of Type Ia and CC SNe at redshift 1.91, generated with the SuperNova ANAlysis software (SNANA;Our procedure gives us a very high probability that SN UDS10Wil is a SN Ia. We discuss the use of spectral evidence for classification of $z > In addition to understanding their explosion physics, the connection between progenitor channels and SN Ia luminosity is of utmost importance for cosmology. The Dark Cosmology Centre is funded by the DNRF. We find that the standard ΛCDM model gives the highest chi-square probability in all cases albeit with a rather small margin over the next best model - the recently introduced nonadiabatic Einstein de Sitter model. The sum of the evidence for a SN Ia model gives a nearly 100% probability that the SN is of Type Ia. Simulations of non–Ia-type SNe are based on spectroscopically confirmed light curves that include unpublished non-Ia samples donated from the Carnegie Supernova Project (CSP), the Supernova Legacy Survey (SNLS), and the Sloan Digital Sky Survey-II (SDSS-II). modifications of Einstein gravity or new forms of energy.
To compare each of the 30,000 synthetic light curves to the CC SNe have greater heterogeneity, such that our relatively small set of discrete templates cannot describe the entire population. The center of the nearest neighboring galaxy, which causes minimal lensing of the SN (see § 4.1), is located ∼ 1 . This sample consists of SN candidates with no spectroscopic confirmation, with a subset of 210 candidates having spectroscopic redshifts of their host galaxies measured while the remaining 860 candidates are purely photometric in their identification. They concluded that their observations and find it to be ~35% lower than our lensing-derived profile at We have made (z-μ) projections up to z=1096 for the best four models. For (2011) found thatFigure 2 shows the best-fit light curves, along withbest-fit light curves for Types Ia, Ib/c, and II SNe re-the final classification probability relies on the weighthat we underestimated the uncertainties), the Type Iathe nearly 100% probability of classification as a SNthe combination of SN UDS10Wil’s high signal-to-noiseratio (S/N) discovery-epoch colors and its rapid light-(PSNID; Sako et al. A suitable definition of this assembly time allows the same proportionality constant to be used for all the cosmologies that we have tested. The Balmer break is between the Subaru z band and the WFC3 J band, making the most likely redshift between 1.8 and 2.2 (see the lower-left panel of Figure 3). 2011, MNRAS, 412, 1441Peng, C. Y., Ho, L. C., Impey, C. D., & Rix, H.-W. 2002, AJ,Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. In the case of SN UDS10Wil, the SN was separated from its host galaxy by only∼0:1′′, contaminating the SN spectrum with host-galaxy light. optical U, B, and V images The expansion of the Universe is accelerated as testified by observations of