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

astro-ph/0309368

Contents:

• Preprint
• Figures
• Summary Data Tables, Probability Distributions
• Lightcurve Data
• Vanderbilt Press Release
• LBNL Press Release

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Preprint

A preprint of this paper is available in PDF format.

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Figures

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.

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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.)

• Table 3 – Lightcurve fit parameters for the 11 HST SNe of this paper.

• Table 4 – Lightcurve fit parameters for supernovae from Perlmutter (1999).

• Table 5 – Lightcurve fit parameters for supernovae from Hamuy (1996) and Riess (1999).

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) {
       om=minom+i*(maxom-minom)/numom;
       ol=minol+j*(maxol-minol)/numol;
       prob=data[i*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.

• fit3_omegalambda.dat
• fit3_omegaw.dat

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.

• fit6_omegalambda.dat
• fig6_omegaw.dat

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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.

Supernova	R-band Data	I-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