# 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

## Preprint

A preprint of this paper is available in PDF format.

## 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.

## 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.

**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.

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 |