Refereed journal article or data article (A1)

A Linear Relation between the Color Stretch sBV and the Rising Color Slope s0*(B−V) of Type Ia Supernovae



List of Authors: 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

Publisher: Institute of Physics

Publication year: 2023

Journal: Astrophysical Journal

Journal name in source: Astrophysical Journal

Article number: 101

Volume number: 946

Issue number: 2

eISSN: 1538-4357

DOI: http://dx.doi.org/10.3847/1538-4357/acc404

URL: https://iopscience.iop.org/article/10.3847/1538-4357/acc404

Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/179565724


Abstract

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 ${s}_{0}^{* }(B-V)$ 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 ${s}_{0}^{* }$. Unlike sBV (or Δm15(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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Last updated on 2023-06-06 at 12:51