The Early Light Curve of SN 2023bee: Constraining Type Ia Supernova Progenitors the Apian Way
G. Hosseinzadeh, David J. Sand, Sumit K. Sarbadhicary, S. D. Ryder, Saurabh W. Jha, Yize Dong, K. Azalee Bostroem, Jennifer E. Andrews, Emily Hoang, Daryl Janzen, J. Jencson, M. Lundquist, N. Meza, Jeniveve Pearson, Manisha Shrestha, S. Valenti, S. Wyatt, Joseph Farah, D. A. Howell, C. McCully, Megan Newsome, Estefania Padilla Gonzalez, C. Pellegrino, G. Terreran, Muzoun Alzaabi, Elizabeth M. Green, Jessica L. Gurney, Peter Milne, Kaycee I. Ridenhour, Nathan Smith, Paulina Soto Robles, Lindsey A. Kwok, Michaela Schwab, M. Gromadzki, D. A. H. Buckley, Koichi 公一 Itagaki 板 垣, D. Hiramatsu, Laura Chomiuk, Peter Lundqvist, J. Haislip, Vladimir Kouprianov, D. Reichart
Abstract
Abstract We present very early photometric and spectroscopic observations of the Type Ia supernova (SN Ia) 2023bee, starting about 8 hr after the explosion, which reveal a strong excess in the optical and nearest UV ( U and UVW1 ) bands during the first several days of explosion. This data set allows us to probe the nature of the binary companion of the exploding white dwarf and the conditions leading to its ignition. We find a good match to the Kasen model in which a main-sequence companion star stings the ejecta with a shock as they buzz past. Models of double detonations, shells of radioactive nickel near the surface, interaction with circumstellar material, and pulsational delayed detonations do not provide good matches to our light curves. We also observe signatures of unburned material, in the form of carbon absorption, in our earliest spectra. Our radio nondetections place a limit on the mass-loss rate from the putative companion that rules out a red giant but allows a main-sequence star. We discuss our results in the context of other similar SNe Ia in the literature.