Details

Autor(en) / Beteiligte

• Lampeitl, H.
• Nichol, R. C.
• Seo, H.-J.
• Giannantonio, T.
• Shapiro, C.
• Bassett, B.
• Percival, W. J.
• Davis, T. M.
• Dilday, B.
• Frieman, J.
• Garnavich, P.
• Sako, M.
• Smith, M.
• Sollerman, J.
• Becker, A.C.
• Cinabro, D.
• Filippenko, A. V.
• Foley, R. J.
• Hogan, C. J.
• Holtzman, J. A.
• Jha, S. W.
• Konishi, K.
• Marriner, J.
• Richmond, M. W.
• Riess, A. G.
• Schneider, D. P.
• Stritzinger, M.
• van der Heyden, K. J.
• VanderPlas, J. T.
• Wheeler, J. C.
• Zheng, C.

Titel

First-year Sloan Digital Sky Survey-II supernova results: consistency and constraints with other intermediate-redshift data sets

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2010-02, Vol.401 (4), p.2331-2342

Ort / Verlag

Oxford, UK: Blackwell Publishing Ltd

Erscheinungsjahr

2010

Quelle

Wiley Online Library

Beschreibungen/Notizen

• We present an analysis of the luminosity distances of Type Ia Supernovae (SNe) from the Sloan Digital Sky Survey-II (SDSS-II) SN Survey in conjunction with other intermediate-redshift (z < 0.4) cosmological measurements including redshift-space distortions from the Two-Degree Field Galaxy Redshift Survey (2dFGRS), the integrated Sachs–Wolfe (ISW) effect seen by the SDSS and the latest baryon acoustic oscillation (BAO) distance scale from both the SDSS and 2dFGRS. We have analysed the SDSS-II SN data alone using a variety of ‘model-independent’ methods and find evidence for an accelerating Universe at a >97 per cent level from this single data set. We find good agreement between the SN and BAO distance measurements, both consistent with a Λ-dominated cold dark matter cosmology, as demonstrated through an analysis of the distance duality relationship between the luminosity (dL) and angular diameter (dA) distance measures. We then use these data to estimate w within this restricted redshift range (z < 0.4). Our most stringent result comes from the combination of all our intermediate-redshift data (SDSS-II SNe, BAO, ISW and redshift-space distortions), giving w=−0.81+0.16−0.18 (stat) ± 0.15 (sys) and ΩM= 0.22+0.09−0.08 assuming a flat universe. This value of w and associated errors only change slightly if curvature is allowed to vary, consistent with constraints from the cosmic microwave background. We also consider more limited combinations of the geometrical (SN, BAO) and dynamical (ISW, redshift-space distortions) probes.