S. Bose, Subo Dong, A. Pastorello, A. V. Filippenko, C. S. Kochanek, Jon C. Mauerhan, Cristina Romero-Cañizales, Thomas G. Brink, Ping Chen, J. L. Prieto, R. S. Post, C. Ashall, D. Grupe, L. Tomasella, S. Benetti, B. J. Shappee, K. Z. Stanek, Zheng Cai, E. Falco, Peter Lundqvist, S. Mattila, R. L. Mutel, P. Ochner, D. Pooley, M. Stritzinger, Steven Villanueva, WeiKang Zheng, R. J. Beswick, P. J. Brown, E. Cappellaro, Scott Davis, M. Fraser, Thomas de Jaeger, N. Elias‐Rosa, C. Gall, B. Scott Gaudi, Gregory J. Herczeg, Julia C. Hestenes, T. W. S. Holoien, G. Hosseinzadeh, E. Y. Hsiao, Shaoming Hu, Jaejin Shin, B. Jeffers, R. A. Koff, S. Kumar, Alexander Kurtenkov, Marie Wingyee Lau, S. Prentice, T. Reynolds, R. J. Rudy, Melissa Shahbandeh, A. Somero, Keivan G. Stassun, Todd A. Thompson, S. Valenti, Jong-Hak Woo, Sameen Yunus,
Hydrogen-poor superluminous supernovae (SLSNe-I) have been predominantly found in low-metallicity, star-forming dwarf galaxies. Here we identify Gaia17biu/SN 2017egm as an SLSN-I occurring in a "normal" spiral galaxy (NGC 3191) in terms of stellar mass (several times 10^10 M_sun) and metallicity (roughly Solar). At redshift z=0.031, Gaia17biu is also the lowest redshift SLSN-I to date, and the absence of a larger population of SLSNe-I in dwarf galaxies of similar redshift suggests that metallicity is ...
Tópico(s): Stellar, planetary, and galactic studies
2018 - IOP Publishing | The Astrophysical Journal