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Chen, Ping; Dong, Subo; Ashall, Chris; Benetti, S.; Bersier, D.; Bose, S.; Brimacombe, Joseph; Brink, Thomas G.; Buckley, David A. H.; Cappellaro, Enrico; Christie, Grant W.; Elias-Rosa, N.; Filippenko, Alexei V.; Gromadzki, Mariusz; Holoien, Thomas W. -S.; Hu, Shaoming; Kochanek, C. S.; Koff, Robert; Kollmeier, Juna A.; Lundqvist, Peter; Mattila, S.; Milne, Peter A.; Muñoz, J. A.; Mutel, Robert; Natusch, Tim; Nicolas, Joel; Pastorello, A.; Prentice, Simon; Prieto, J. L.; Roth, Tyler; Shappee, B. J.; Stone, Geoffrey; Stanek, K. Z.; Stritzinger, M. D.; Thompson, Todd A.; Tomasella, Lina; Villanueva, Steven
The Astrophysical journal, 2023, Letnik: 946, Številka: 2Journal Article
Using data from the Complete Nearby (redshift z host < 0.02) sample of Type Ia Supernovae (CNIa0.02), we find a linear relation between two parameters derived from the B − V color curves of Type Ia supernovae: the color stretch s BV and the rising color slope s 0 * (B – V) after the peak, and this relation applies to the full range of s BV . The s BV parameter is known to be tightly correlated with the peak luminosity, especially for fast decliners (dim Type Ia supernovae), and the luminosity correlation with s BV is markedly better than with the classic light-curve width parameters such as Δm 15 (B). Thus, our new linear relation can be used to infer peak luminosity from s 0 * . Unlike s BV (or Δm 15 (B)), the measurement of s 0 * (B – V) does not rely on a well-determined time of light-curve peak or color maximum, making it less demanding on the light-curve coverage than past approaches.
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in: SICRIS
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