Measurements of Omega and Lambda from 42 High-Redshift Supernovae
read more
Citations
Seven-year wilkinson microwave anisotropy probe (wmap *) observations: cosmological interpretation
Planck 2015 results - XIII. Cosmological parameters
First year Wilkinson Microwave Anisotropy Probe (WMAP) observations: Determination of cosmological parameters
Planck 2013 results. XVI. Cosmological parameters
Wilkinson Microwave Anisotropy Probe (WMAP) three year results: implications for cosmology
References
Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant To Appear in the Astronomical Journal
Cosmological imprint of an energy component with general equation of state
Unified approach to the classical statistical analysis of small signals
Quintessence, cosmic coincidence, and the cosmological constant
The keck low-resolution imaging spectrometer
Related Papers (5)
Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant
First year Wilkinson Microwave Anisotropy Probe (WMAP) observations: Determination of cosmological parameters
Type Ia supernova discoveries at z > 1 from the Hubble Space Telescope: Evidence for past deceleration and constraints on dark energy evolution
Frequently Asked Questions (11)
Q2. What are the future works in this paper?
Thus the universe may be Ñat or there may be little or no cosmological constant, but the data are not consistent with both possibilities simultaneously. 2. presented here and future complementary data sets will allow us to explore these possibilities. For their purposes here the authors wish to distinguish between the true probability distribution, P ( A ), and its estimated or assumed distribution, often called the Bayesian prior, which they denote as P ( A ). Third, even if the universe is not Ñat, the conÐdence regions of Figure 7 suggest that the cosmological constant is a signiÐcant constituent of the energy density of the universe.
Q3. What is the appropriate measure to compare with their results?
Since there is evidence that dynamical estimates of depend on scale, the most appropriate measures to) Mcompare with their result are those obtained on large scales.
Q4. What is the possibility of a strong metallicity eect?
The consistency of slopes in the light-curve widthluminosity relation for the low- and high-redshift supernovae can also constrain the possibility of a strong metallicity e†ect of the type that et al.
Q5. Why is the total systematic uncertainty a separate analysis case?
due to small-scale clumping of mass as a separate analysis case rather than as a contributing systematic error in their primary analysis ; the total systematic uncertainty applies to this analysis as well.
Q6. What is the stretch factor used to determine the light curves of the Cala n/?
at high redshift the rest-frame B-band photometry is usually much more densely sampled in time than the rest-frame V -band data, so the authors use the stretch factor that best
Q7. What is the extinction probability distribution implied by the measured colorexcess?
In brief, in this method the Gaussian extinction probability distribution implied by the measured colorexcess and its error is multiplied by an assumed a priori probability distribution (the Bayesian prior) for the intrinsic distribution of host extinctions.
Q8. What is the difference between the rest-frame color and the stretch factor?
Since there is a small dependence of intrinsic color on the light-curve width, supernova colors can only be compared for the same stretch factor ; for a more convenient analysis, the authors subtract out the intrinsic colors so that the remaining color excesses can be compared simultaneously for all stretch factors.
Q9. What is the best-t mass density in a at universe?
The best-Ðt mass-density in a Ñat universe for Ðt A is, within a fraction of the uncertainty, the same value as for Ðt B, (see Table 3).
Q10. What is the t for the age of the universe for these analyses?
The best Ðts for the age of the universe for these analyses are H0 t0\\and To Ðrst order, the Reiss et0.90~0.05`0.07 H0 t0\\ 0.98~0.05`0.07.al.
Q11. What are the two coincidences that must be addressed in future cosmological theories?
If in fact the universe has a dominant energy contribution from a cosmological constant, there are two coincidences that must be addressed in future cosmological theories.