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

Ping Chen; Subo Dong; Chris Ashall; S. Benetti; D. Bersier; S. Bose; Joseph Brimacombe; Thomas G. Brink; David A.H. Buckley; Enrico Cappellaro; Grant W. Christie; N. Elias-Rosa; Alexei V. Filippenko; Mariusz Gromadzki; Thomas W.S. Holoien; Shaoming Hu; C. S. Kochanek; Robert Koff; Juna A. Kollmeier; P. Lundqvist; S. Mattila; Peter A. Milne; J. A. Muñoz; Robert Mutel; Tim Natusch; Joel Nicolas; A. Pastorello; Simon Prentice; J. L. Prieto; Tyler Roth; B. J. Shappee; Geoffrey Stone; K. Z. Stanek; M. D. Stritzinger; Todd A. Thompson; Lina Tomasella; Steven Villanueva

doi:10.3847/1538-4357/acc404

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

Ping Chen, Subo Dong, Chris Ashall, S. Benetti, D. Bersier, S. Bose, Joseph Brimacombe, Thomas G. Brink, David A.H. Buckley, Enrico Cappellaro, Grant W. Christie, N. Elias-Rosa, Alexei V. Filippenko, Mariusz Gromadzki, Thomas W.S. Holoien, Shaoming Hu, C. S. Kochanek, Robert Koff, Juna A. Kollmeier, P. LundqvistS. Mattila, Peter A. Milne, J. A. Muñoz, Robert Mutel, Tim Natusch, Joel Nicolas, A. Pastorello, Simon Prentice, J. L. Prieto, Tyler Roth, B. J. Shappee, Geoffrey Stone, K. Z. Stanek, M. D. Stritzinger, Todd A. Thompson, Lina Tomasella, Steven Villanueva

Steward Observatory

Research output: Contribution to journal › Article › peer-review

Abstract

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.

Original language	English (US)
Article number	101
Journal	Astrophysical Journal
Volume	946
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/acc404
State	Published - Apr 1 2023

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/acc404

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Chen, P., Dong, S., Ashall, C., Benetti, S., Bersier, D., Bose, S., Brimacombe, J., Brink, T. G., Buckley, D. A. H., Cappellaro, E., Christie, G. W., Elias-Rosa, N., Filippenko, A. V., Gromadzki, M., Holoien, T. W. S., Hu, S., Kochanek, C. S., Koff, R., Kollmeier, J. A., ... Villanueva, S. (2023). A Linear Relation between the Color Stretch s_BV and the Rising Color Slope s₀*(B−V) of Type Ia Supernovae. Astrophysical Journal, 946(2), Article 101. https://doi.org/10.3847/1538-4357/acc404

Chen, P, Dong, S, Ashall, C, Benetti, S, Bersier, D, Bose, S, Brimacombe, J, Brink, TG, Buckley, DAH, Cappellaro, E, Christie, GW, Elias-Rosa, N, Filippenko, AV, Gromadzki, M, Holoien, TWS, Hu, S, Kochanek, CS, Koff, R, Kollmeier, JA, Lundqvist, P, Mattila, S, Milne, PA, Muñoz, JA, Mutel, R, Natusch, T, Nicolas, J, Pastorello, A, Prentice, S, Prieto, JL, Roth, T, Shappee, BJ, Stone, G, Stanek, KZ, Stritzinger, MD, Thompson, TA, Tomasella, L & Villanueva, S 2023, 'A Linear Relation between the Color Stretch s_BV and the Rising Color Slope s₀*(B−V) of Type Ia Supernovae', Astrophysical Journal, vol. 946, no. 2, 101. https://doi.org/10.3847/1538-4357/acc404

@article{6ea00c94ec4147198d7a2a7359c20daf,

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

abstract = "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.",

author = "Ping Chen and Subo Dong and Chris Ashall and S. Benetti and D. Bersier and S. Bose and Joseph Brimacombe and Brink, {Thomas G.} and Buckley, {David A.H.} and Enrico Cappellaro and Christie, {Grant W.} and N. Elias-Rosa and Filippenko, {Alexei V.} and Mariusz Gromadzki and Holoien, {Thomas W.S.} and Shaoming Hu and Kochanek, {C. S.} and Robert Koff and Kollmeier, {Juna A.} and P. Lundqvist and S. Mattila and Milne, {Peter A.} and Mu{\~n}oz, {J. A.} and Robert Mutel and Tim Natusch and Joel Nicolas and A. Pastorello and Simon Prentice and Prieto, {J. L.} and Tyler Roth and Shappee, {B. J.} and Geoffrey Stone and Stanek, {K. Z.} and Stritzinger, {M. D.} and Thompson, {Todd A.} and Lina Tomasella and Steven Villanueva",

note = "Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

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doi = "10.3847/1538-4357/acc404",

language = "English (US)",

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T1 - A Linear Relation between the Color Stretch sBV and the Rising Color Slope s0*(B−V) of Type Ia Supernovae

AU - Chen, Ping

AU - Dong, Subo

AU - Ashall, Chris

AU - Benetti, S.

AU - Bersier, D.

AU - Bose, S.

AU - Brimacombe, Joseph

AU - Brink, Thomas G.

AU - Buckley, David A.H.

AU - Cappellaro, Enrico

AU - Christie, Grant W.

AU - Elias-Rosa, N.

AU - Filippenko, Alexei V.

AU - Gromadzki, Mariusz

AU - Holoien, Thomas W.S.

AU - Hu, Shaoming

AU - Kochanek, C. S.

AU - Koff, Robert

AU - Kollmeier, Juna A.

AU - Lundqvist, P.

AU - Mattila, S.

AU - Milne, Peter A.

AU - Muñoz, J. A.

AU - Mutel, Robert

AU - Natusch, Tim

AU - Nicolas, Joel

AU - Pastorello, A.

AU - Prentice, Simon

AU - Prieto, J. L.

AU - Roth, Tyler

AU - Shappee, B. J.

AU - Stone, Geoffrey

AU - Stanek, K. Z.

AU - Stritzinger, M. D.

AU - Thompson, Todd A.

AU - Tomasella, Lina

AU - Villanueva, Steven

PY - 2023/4/1

Y1 - 2023/4/1

N2 - 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.

AB - 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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DO - 10.3847/1538-4357/acc404

M3 - Article

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SN - 0004-637X

VL - 946

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 101

ER -

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

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