New Constraints on ΩM, ΩΛ, and w from an Independent Set of Eleven High-Redshift Supernovae Observed with HST


Knop et al (The Supernova Cosmology Project)

The Astrophysical Journal, 2003, 598, 102




A preprint of this paper is available in PDF format.


When using any of these figures in talks or elsewhere, include a citation to "Knop et. al. 2003, ApJ, 598, 102"

Figures below are presented in two formats. Click on the thumbnail image to get an EPS (Encapsulated Postscript) image. As a vector format, this is what you will want to use if you print anything out. Each figures also has a PNG image available, which is what you would use in a computer presentation. Their resolution is such that while they are fine for this, they will look jagged when printed out.

Summary Data Tables, Probability Distributions

Summary Data Tables

These are data tables with the information in Tables 3-5 from the paper. The columns are in the same order as the columns in the paper; see the paper for their meanings. (Note that uncertainties on numbers provided in the table the paper are in an additional column after the number to which they apply.)

Probability Distributions

These files give the probability denstiy functions from our chi-square fits to cosmological models. Each file is written as a series of little-endian double-precision IEEE values. (If you are on a Linux x86 system, and read these using standard I/O functions, the double values will be read in properly. If you are on a big-endian system, e.g. a Solaris Sparc, you will need to perform an endianness conversion.) The format of the files is as follows:

   double minom;
   double maxom;
   double numom;
   double minol
   double maxol;
   double numol;
   double data[numom*numol];

(For Omega/w probability distributions, substitute "w" for "ol" above.) To figure out what values of the cosmological parameters a given element of the data array corresponds to, use code similar to the following:

   int i,j;
   double om,ol,prob

   for (i=0 ; i<(int)numom ; ++i) {
     for (j=0 ; j<(int)numol ; ++j) {
       /* Do something with om, ol, and prob */
Fit 3

This is a fit to the low-extinction subset, and is the primary fit from the paper. It is what is plotted in Figure 8, and in the left panels of Figure 12.

Fit 6

This is a fit with extinction-corrections applied to the full primary subset. It is what is plotted in the bottom-right panel of Figure 10, and in the right column of Figure 12.

Lightcurve Data

These are equivalent to the data tables from the appendix, only with the covariance matrices included. The format of the file should be self-explanatory. The first line gives the effective zeropoint; all zeropoint uncertainties have been included in the covariance matrix. Add 2,400,000 to the "jd" column to get the Julian date of a data point. The covariance matrix comes in the form of a list of datapoints^2 numbers; because it is symmetric, you need not worry about row/column ordering.

SupernovaR-band DataI-band Data
1997ek 1997ek-R.dat 1997ek-I.dat
1997eq 1997eq-R.dat 1997eq-I.dat
1997ez 1997ez-R.dat 1997ez-I.dat
1998as 1998as-R.dat 1998as-I.dat
1998aw 1998aw-R.dat 1998aw-I.dat
1998ax 1998ax-R.dat 1998ax-I.dat
1998ay 1998ay-R.dat 1998ay-I.dat
1998ba 1998ba-R.dat 1998ba-I.dat
1998be 1998be-R.dat 1998be-I.dat
1998bi 1998bi-R.dat 1998bi-I.dat
2000fr 2000fr-R.dat 2000fr-I.dat