No Access Published Online: 15 November 2010
AIP Conference Proceedings 1294, 268 (2010); https://doi.org/10.1063/1.3518871
more...View Affiliations
• aInstitute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwanoha 5‐1‐5, Kashiwa, Chiba 277‐8583, Japan
• bDepartment of Astronomy and Recearch Center for the Early Universe, Graduate School of Science, University of Tokyo, Bunkyo‐ku, Tokyo 113‐0033, Japan
• cDepartment of Physics, Faculty of Science and Engineering, Konan University, 8‐9‐1 Okamoto, Kobe, Hyogo 658‐8501, Japan
• dInstitute for Theoretical and Experimental Physics, Moscow, 117218, Russia
View Contributors
• Takashi Moriya
• Naoki Yoshida
• Nozomu Tominaga
• Sergei I. Blinnikov
• Keiichi Maeda
• Masaomi Tanaka
• Ken’ichi Nomoto
A supernova (SN) becomes as bright as a galaxy and is a powerful tool for probing the high‐redshift universe. In particular, it has been suggested that extremely luminous SNe $(MR<−21)$ are detectable at z>2, which is difficult for type Ia SNe. Some luminous SNe, such as type IIn SNe, are believed to be powered by the interaction of the SN ejecta with the circumstellar medium. One of the interesting features of interaction‐powered SNe is the fact that they are bright in UV. With their intrinsic brightness in UV, interaction‐powered SNe could unveil the properties of stars at high redshift and probe the primordial universe. We performed multigroup light curve calculations of interaction‐powered SNe using the STELLA code. Based on the synthetic multicolor light curves, we estimate the detectability of interaction‐powered SNe at high redshifts with several telescopes.
1. © 2010 American Institute of Physics.