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Luminosity-Dependent Variations in the Secondary Maximum of Type Ia Supernovae and Their Connection to Host Galaxy Morphology

Jagriti Gaba, Rahul Kumar Thakur, Dinkar Verma, Naresh Sharma, Shashikant Gupta

Abstract

Type Ia supernovae (SNe Ia) are considered standardizable candles and are therefore important probes of the universe's expansion history and cosmic distances. In comparison to the optical and IR photometric observations, NIR light curves of SNe Ia are more uniform and are less affected by dust extinction; hence, they can provide more precise distance estimates. This study examines the relationship between the luminosity-dependent behavior of the NIR secondary maximum ($t_2$) and the decline rate parameter ($Δm_{15}$) in the B Band. We analyzed 54 SNe Ia using linear, piecewise linear regression, and non-linear models along with non-parametric statistical techniques to examine the correlation between $t_2$ and $Δm_{15}$. Our results show that the secondary maximum timing varies among SNe Ia but exhibits a luminosity-dependent structure, with significant differences between SNe hosted in late and early-type galaxies. Two separate groups belonging to different host morphologies have been identified through our analysis, one containing brighter SNe and the other containing fainter SNe. These findings have important implications for improving the calibration of SNe Ia for cosmological applications.

Luminosity-Dependent Variations in the Secondary Maximum of Type Ia Supernovae and Their Connection to Host Galaxy Morphology

Abstract

Type Ia supernovae (SNe Ia) are considered standardizable candles and are therefore important probes of the universe's expansion history and cosmic distances. In comparison to the optical and IR photometric observations, NIR light curves of SNe Ia are more uniform and are less affected by dust extinction; hence, they can provide more precise distance estimates. This study examines the relationship between the luminosity-dependent behavior of the NIR secondary maximum () and the decline rate parameter () in the B Band. We analyzed 54 SNe Ia using linear, piecewise linear regression, and non-linear models along with non-parametric statistical techniques to examine the correlation between and . Our results show that the secondary maximum timing varies among SNe Ia but exhibits a luminosity-dependent structure, with significant differences between SNe hosted in late and early-type galaxies. Two separate groups belonging to different host morphologies have been identified through our analysis, one containing brighter SNe and the other containing fainter SNe. These findings have important implications for improving the calibration of SNe Ia for cosmological applications.
Paper Structure (13 sections, 18 equations, 2 figures, 5 tables)

This paper contains 13 sections, 18 equations, 2 figures, 5 tables.

Table of Contents

  1. Introduction
  2. Data and Methodology
  3. Data
  4. Methodology
  5. Piece-wise Linear Regression and Non-linear Modeling
  6. Comparison of the Models
  7. Mann-Whitney U Test
  8. Results and Discussion
  9. Piecewise Linear Regression Analysis and Non-linear Model
  10. Host Galaxy Morphology and the Mann-Whitney U Test
  11. Conclusion
  12. Cluster Analysis Using Hierarchical Clustering Technique and Gower Distance
  13. SNe Ia Data

Figures (2)

  • Figure 1: Comparison of linear, quadratic, and piecewise regression models fitted to the data.
  • Figure 1: Hierarchical clustering dendrogram of Type Ia supernovae based on their photometric properties, constructed using the average linkage method. The vertical axis represents the distance or dissimilarity between clusters. The branching pattern reveals the hierarchical relationship among supernovae and suggests natural groupings based on similarities in their decline rates and secondary maximum characteristics.