ZTF SN Ia DR2: Secondary maximum in type Ia supernovae

Type Ia supernova (SN Ia) light curves have a secondary maximum that exists in the r , i , and near-infrared filters. The secondary maximum is relatively weak in the r band, but holds the advantage that it is accessible, even at high redshift. We used Gaussian process fitting to parameterise the light curves of 893 SNe Ia from the Zwicky Transient Facility’s (ZTF) second data release (DR2), and we were able to extract information about the timing and strength of the secondary maximum. We found > 5 σ correlations between the light curve dec rate (Δ m 15 ( g )) and the timing and strength of the secondary maximum in the r band. Whilst the timing of the secondary maximum in the i band is also correlated with Δ m 15 ( g ), the strength of the secondary maximum in the i band shows significant scatter as a function of Δ m 15 ( g ). We found that the transparency timescales of 97 per cent of our sample are consistent with double detonation models and that SNe Ia with small transparency timescales (< 32 d) reside predominantly in locally red environments. We measured the total ejected mass for the normal SNe Ia in our sample using two methods and both were consistent with medians of 1.3 ± 0.3 and 1.2 ± 0.2 M ⊙ . We find that the strength of the secondary maximum is a better standardisation parameter than the SALT light curve stretch ( x 1 ). Finally, we identified a spectral feature in the r band as Fe II , which strengthens during the onset of the secondary maximum. The same feature begins to strengthen at < 3 d post maximum light in 91bg-like SNe. Finally, the correlation between x 1 and the strength of the secondary maximum was best fit with a broken, with a split at x 1 0 = − 0.5 ± 0.2, suggestive of the existence of two populations of SNe Ia.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2024-08-19
DOI
https://doi.org/10.1051/0004-6361/202450379
Citations
4
Primary Topic
Gamma-ray bursts and supernovae
Type
article
Field-Weighted Citation Impact
1.33

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article

ZTF SN Ia DR2: Secondary maximum in type Ia supernovae

Luke J. Shingles, F. J. Masci, M. Deckers, M Ginolin et al.
4 citations
Astronomy and Astrophysics
Gamma-ray bursts and supernovae
1.33
article

ZTF SN Ia DR2: Secondary maximum in type Ia supernovae

Luke J. Shingles, F. J. Masci, M. Deckers, M Ginolin, Young-Lo Kim, M. R. Smith, T. E. Müller-Bravo, S. R. Kulkarni, Suhail Dhawan, Lisa A. Harvey, W. D. Kenworthy, J. Sollerman, K. Maguire, J. H. Terwel, M. Rigault, G. Dimitriadis, Russ R. Laher, P. Nugent, J. Purdum, J. Nordin, M. Amenouche, J. Johansson, U. Burgaz, Natalya Pletskova, B. Racine, N. Luo, A. Goobar
article en
4 citations

Abstract

Type Ia supernova (SN Ia) light curves have a secondary maximum that exists in the r , i , and near-infrared filters. The secondary maximum is relatively weak in the r band, but holds the advantage that it is accessible, even at high redshift. We used Gaussian process fitting to parameterise the light curves of 893 SNe Ia from the Zwicky Transient Facility’s (ZTF) second data release (DR2), and we were able to extract information about the timing and strength of the secondary maximum. We found > 5 σ correlations between the light curve dec rate (Δ m 15 ( g )) and the timing and strength of the secondary maximum in the r band. Whilst the timing of the secondary maximum in the i band is also correlated with Δ m 15 ( g ), the strength of the secondary maximum in the i band shows significant scatter as a function of Δ m 15 ( g ). We found that the transparency timescales of 97 per cent of our sample are consistent with double detonation models and that SNe Ia with small transparency timescales (< 32 d) reside predominantly in locally red environments. We measured the total ejected mass for the normal SNe Ia in our sample using two methods and both were consistent with medians of 1.3 ± 0.3 and 1.2 ± 0.2 M ⊙ . We find that the strength of the secondary maximum is a better standardisation parameter than the SALT light curve stretch ( x 1 ). Finally, we identified a spectral feature in the r band as Fe II , which strengthens during the onset of the secondary maximum. The same feature begins to strengthen at < 3 d post maximum light in 91bg-like SNe. Finally, the correlation between x 1 and the strength of the secondary maximum was best fit with a broken, with a split at x 1 0 = − 0.5 ± 0.2, suggestive of the existence of two populations of SNe Ia.

Astronomy and AstrophysicsVol. 694
Université Claude Bernard Lyon 1 (FR), California Institute of Technology (US), Herzberg Institute of Astrophysics (CA), Centre National de la Recherche Scientifique (FR), Institute of Space Sciences (ES), Lawrence Berkeley National Laboratory (US), Stockholm University (SE), GSI Helmholtz Centre for Heavy Ion Research (DE), Lyon College (US), Trinity College Dublin (IE), Aix-Marseille Université (FR), University of Cambridge (GB), Humboldt-Universität zu Berlin (DE), Institut d'Estudis Espacials de Catalunya (ES), Infrared Processing and Analysis Center (US), Lancaster University (GB), Drexel University (US), University of California, Berkeley (US)
National Science Foundation, California Institute of Technology, Northwestern University, University of Washington, Heising-Simons Foundation, University of Warwick, European Commission, Trinity College Dublin, Deutsche Forschungsgemeinschaft, Weizmann Institute of Science, Irish Research Council, Generalitat de Catalunya, Knut och Alice Wallenbergs Stiftelse, Vetenskapsrådet, Ministerio de Ciencia e Innovación, Stockholms Universitet, Horizon 2020 Framework Programme, Science and Technology Facilities Council, Deutsches Elektronen-Synchrotron, Agencia Estatal de Investigación, Institut National de Physique Nucléaire et de Physique des Particules, HORIZON EUROPE European Research Council
Openalex Percentile: Top 20%
Gamma-ray bursts and supernovae
1.33
DOIOpen Access PDFOpenAlex
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