AAS 205th Meeting, 9-13 January 2005
Session 71 Supernovae
Poster, Tuesday, January 11, 2005, 9:20am-6:30pm, Exhibit Hall

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[71.15] A Set of Nearby SNe Ia Lightcurves

M. Kowalski, G. Aldering, A. Conley, B. Farris, V. Fadeyev, B. Frye, R. Gibbons, G. Goldhaber, D.E. Groom, D.A. Howell, D. Kasen, A.G. Kim, B.C. Lee, P.E. Nugent, S. Perlmutter, V. Prasad, R. Quimby, N. Regnault, A.L. Spadafora, R.C. Thomas, L. Wang, W.M. Wood-Vasey (LBNL), A. Amadon (DAPNIA, Saclay), R. Amanullah, G. Folatelli, G. Garavini, A. Goobar, S. Nobili, V. Stanishev (Stockholm U.), P. Astier, D. Hardin, R. Pain, J. Raux, G. Sainton, K. Schahmaneche (U. Paris VI & VII), C. Balland (U. Paris VI & VII & Sud), G. Blanc (LBNL, Osserva. Astro. di Padova), M.S. Burns (Colorado Coll.), T. Dahlén (Stockholm Obs., STSI), S.E. Deustua (LBNL, AAS), R. Ellis (Caltech), S. Fabbro, A. Mour (IST, Lisbon), X. Fan (Steward Obs., U. Arizona), E.L. Gates (Lick Obs.), B. Goldman (NMSU), J. Haissinski, M. Moniez (Université Paris Sud), I.M. Hook, O. Perdereau (U. Oxford), S. Kent (FNAL), R.A. Knop, E. Smith (Vanderbilt U.), C. Lidman (ESO), J. Mendez (ING, U. Barcelona), G.J. Miller (SDSU, U. Illinois), H. Newberg (RPI), J. Rich (DAPNIA, Saclay), G.T. Richards, B.E. Schaefer (LSU), P. Ruiz-Lapuente (U. Barcelona), N.A. Walton (Cambridge)

Type Ia SNe represent the best distance indicators for cosmology, having established the presence of dark energy through measurement of the expansion history of the universe. While high-z SNe are used to study the change in the expansion rate, low-z SNe establish a baseline for brightness comparisons and provide the important calibration used for standardization. Besides the statistical gain in precision from a large number of SNe, a good understanding of their systematic variations is essential. We present the B, V, R, I lightcurves for a new sample of nearby supernova, obtained by the Supernova Cosmology Project in collaboration with several other supernova groups. A unique challenge of this dataset is that seventeen different instruments were used to obtain the follow-up photometry. Therefore, we focus in particular on the analysis procedure developed for handling and cross-calibrating the data from various instruments.

This work was supported in part by the U.S. Department of Energy under Contract No. DE-AC03-76SF00098.

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