[40.04] Nearby Supernova Factory Observations of the Type Ia Supernova 2004dt

AAS 205th Meeting, 9-13 January 2005
Session 40 SNe Observations and GRB Milky Way Effects
Oral, Monday, January 10, 2005, 2:00-3:30pm, California

Previous | Session 40 | Next

[40.04] Nearby Supernova Factory Observations of the Type Ia Supernova 2004dt

R. C. Thomas, G. Aldering, B. C. Lee, S. Loken, P. Nugent, S. Perlmutter, R. A. Scalzo, J. Siegrist, L. Wang, W. M. Wood-Vasey (LBNL), G. Adam, R. Bacon, C. Bonnaud, L. Capoani, D. Dubet, F. Henault, B. Lantz, J.-P. Lemonnier, A. Pecontal, E. Pecontal (CRAL), N. Blanc, G. Boudoul, S. Bongard, A. Castera, Y. Copin, E. Gangler, G. Smadja (IPNL), R. Kessler (KICP), P. Antilogus, P. Astier, E. Barrelet, G. Garavini, S. Gilles, L.-A. Guevara, D. Imbault, C. Juramy, R. Pain, R. Taillet, D. Vincent (LPNHE), C. Baltay, D. Rabinowitz, J. Snyder (Yale)

The Nearby Supernova Factory has followed the Type Ia supernova 2004dt since its discovery over four months ago. Spectroscopic and photometric data have been collected every two to three days, with wavelength coverage from 320 to 1000 nm. Additional data on SN 2004dt include UV spectroscopy with HST, near-IR spectroscopy with NIRSPEC on the Keck telescope, and spectropolarimetry from the VLT and Subaru telescopes. These data comprise one of the most complete sets of observations of a SN Ia ever obtained, and reveal that SN 2004dt possesses several distinctive spectroscopic features: Very strong \ion{Si}{2}, \ion{Mg}{2}, and \ion{S}{2} lines and a near absence of \ion{Fe}{2} and \ion{Ca}{2} at early times. The data allow detailed studies of the kinematic structure of SN 2004dt, providing important constraints on various SN Ia explosion models.

Support for the SNfactory is provided in the United States by the DOE Office of Science, the Gordon and Betty Moore Foundation, the National Science Foundation through the High Performance Wireless Research and Education Network, and the Kavli Institute for Cosmological Physics, and in France by the Centre National de la Recherche Scientifique (CNRS) through the Institut National de Physique Nucleaire et de Physique des Particules (IN2P3), the Institut National des Sciences de l'Univers (INSU) and the Programme National de Cosmologie (PNC).

If you would like more information about this abstract, please follow the link to http://snfactory.lbl.gov. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

Previous | Session 40 | Next