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A Linear Relation between the Color Stretch sBV and the Rising Color Slope s0*(B−V) of Type Ia Supernovae
Tekijät: 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 P., 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
Kustantaja: Institute of Physics
Julkaisuvuosi: 2023
Journal: Astrophysical Journal
Tietokannassa oleva lehden nimi: Astrophysical Journal
Artikkelin numero: 101
Vuosikerta: 946
Numero: 2
eISSN: 1538-4357
DOI: https://doi.org/10.3847/1538-4357/acc404
Verkko-osoite: https://iopscience.iop.org/article/10.3847/1538-4357/acc404
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/179565724
Using data from the Complete Nearby (redshift zhost < 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 sBV and the rising color slope after the peak, and this relation applies to the full range of sBV. The sBV parameter is known to be tightly correlated with the peak luminosity, especially for fast decliners (dim Type Ia supernovae), and the luminosity correlation with sBV is markedly better than with the classic light-curve width parameters such as Δm15(B). Thus, our new linear relation can be used to infer peak luminosity from
. Unlike sBV (or Δm15(B)), the measurement of
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.
Ladattava julkaisu This is an electronic reprint of the original article. |  |
