Improved cosmological constraints from a joint analysis of the SDSS-II and SNLS supernova samples

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Volume 568 (August 2014)

A&A, 568 (2014) A22

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Table 4

Internal calibration uncertainties for the low-z samples split by photometric systems.

Instrument

Standard^h

Keplercam^h

4Shooter^h

SWOPE^h

Band

σ(λ_eff)^a (nm)

2.5^c

1.2^c

2.5^c

0.7^c

2.5^c

0.7^c

0.7^d

0.8^d

0.4^d

0.2^d

0.7^d

0.3^d

^b (mmag)

100^g

15^c

31^f

11^c

7^c

25^f

7^c

70^g

11^c

7^c

20^c

23^e

9^e

8^e

7^e

8^e

Notes.

^(a)

Uncertainty in the mean filter wavelength.

^(b)

Internal sources of systematic uncertainty in the calibration. It includes the uncertainty in the calibration transfer between secondary and tertiary standards and systematic uncertainties in the SN photometry. For measurements reported in the Landolt system, it also includes an uncertainty associated to the color transformation of supernovae from the observer’s system.

^(c)

From C11.

^(d)

Includes the uncertainties on the new measurement of SWOPE transmission curves presented in Stritzinger et al. (2011) plus the effect of a 0.25 airmass change on the atmospheric extinction curve.

^(e)

From Mosher et al. (2012).

^(f)

See Appendix B.1.

^(g)

See Appendix B.2.

^(h)

Keplercam and 4Shooter are the two main photometric instruments used in the CfAIII survey. SWOPE is the photometric instrument of the CSP survey. We refer to the Landolt photometric system in which the historical measurements are color transformed as the “standard” instrument.

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