AAS 199th meeting, Washington, DC, January 2002
Session 16. Cosmology and Lensing
Display, Monday, January 7, 2002, 9:20am-6:30pm, Exhibit Hall

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[16.12] Results from Recent High-redshift Type Ia Supernovae Searches

K. Schahmaneche (LPNHE), G. Aldering (LBNL), R. Amanullah (Stockholm), P. Antilogus (IPN Lyon), P. Astier (LPNHE), C. Balland (IAS Orsay), G. Blanc (LBNL), M.S. Burns (Colorado Col.), A. Conley, S. Deustua (LBNL), M. Doi (Tokyo), R. Ellis (Caltech), S. Fabbro (IPN Lyon), G. Folatelli (Stockholm), A. Fruchter (STScI), G. Garavini (Stockholm), R. Gibbons, G. Goldhaber (LBNL), A. Goobar (Stockholm), D.E. Groom (LBNL), D. Hardin (LPNHE), I.M. Hook (Oxford), D.A. Howell (LBNL), M. Irwin (IoA Cambridge), D. Kasen, A. Kim, M. Kim (LBNL), R.A. Knop (Vanderbilt), J.C. Lee (MIT ), J.-M. Levy (LPNHE), C. Lidman (ESO), R. McMahon (IoA Cambridge), M. Mouchet (DAEC Meudon), S. Nobili (Stockholm), P. Nugent (LBNL), R. Pain (LPNHE), N. Panagia (STScI), E. Pécontal (CRA Lyon), C.R. Pennypacker, S. Perlmutter, R. Quimby (LBNL), J. Raux (LPNHE), N. Regnault (LBNL), P. Ruiz-Lapuente (Barcelona), B. Schaefer (Texas), A.L. Spadafora (LBNL), N. Walton (ING LaPalma), L. Wang, W.M. Wood-Vasey (LBNL), N. Yasuda (NOA Japan), Supernova Cosmology Project Collaboration

Distant type~Ia supernovae have been used as calibrated standard candles out to z=0.8 (\bar{z} ~q 0.55) to measure the combination ~\Omega\rm M - \Omega\Lambda using the classical magnitude-redshift relation. Extending the redshift range will reduce and eventually break the (\Omega\rm M,\Omega\Lambda) degeneracy, and also discriminate between a non-zero cosmological constant and models of hypothetical intergalactic grey dust. We present here preliminary results from the most recent very high-redshift (z~1) Type Ia supernova searches of the Supernova Cosmology Project. The supernovae were discovered at the CFHT 3.6-m telescope using the CFH12k camera (run in queue mode), the CTIO 4-m telescope using the MOSAIC camera and the Subaru 8.2-m telescope using SuprimeCam. The observations were coordinated with spectroscopic follow-up at Keck, VLT, and Subaru. The optical photometric follow-up was obtained at WIYN, WHT, and TNG for the brighter supernovae, and at HST for the faintest supernovae. The VLT and Gemini made possible the near-IR photometric follow up.

This work was supported in part by the NASA Space Telescope Science Institute.

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