ZTF SN Ia DR2 : High-velocity components in the SiII λ 6355

Harvey, L. and Maguire, K. and Burgaz, U. and Dimitriadis, G. and Sollerman, J. and Goobar, A. and Johansson, J. and Nordin, J. and Rigault, M. and Smith, M. and Aubert, M. and Cartier, R. and Chen, P. and Deckers, M. and Dhawan, S. and Galbany, L. and Ginolin, M. and Kenworthy, W.D. and Kim, Y.-L. and Liu, C. and Miller, A.A. and Rosnet, P. and Senzel, R. and Terwel, J.H. and Tomasella, L. and Kasliwal, M. and Laher, R.R. and Purdum, J. and Rusholme, B. and Smith, R. (2025) ZTF SN Ia DR2 : High-velocity components in the SiII λ 6355. Astronomy and Astrophysics, 695: A264. ISSN 1432-0746

Abstract

The Zwicky Transient Facility SN Ia Data Release 2 provides a perfect opportunity to perform a thorough search for and subsequent analysis of Si IIλ6355 high-velocity features (HVFs) in the pre-peak regime. The source of such features remains unclear, but potential origins include circumstellar material, as well as enhancements to the abundances or densities intrinsic to the supernova (SN) ejecta. Therefore, they may provide clues to the elusive progenitor and explosion scenarios of Type Ia SNe (SNe Ia). We employed a Markov chain Monte Carlo fitting method followed by Bayesian information criterion testing to classify single and double Si IIλ6355 components in the DR2. The detection efficiency of our classification method was investigated through the fitting of simulated features, which allowed us to place cuts on the spectral quality required for reliable classification. These simulations were also used to perform an analysis of the recovered parameter uncertainties and potential biases in the measurements. Within the 329 spectra sample we investigated, we identified 85 spectra exhibiting Si IIλ6355 HVFs. We find that HVFs decrease in strength with phase relative to their photospheric counterparts; however, this decrease can occur at different phases for different objects. HVFs with larger velocity separations from the photosphere were observed to fade earlier, leaving only the double components with smaller separations as we moved towards maximum light. Our findings suggest that around three quarters of SN Ia spectra before −11 d show high-velocity components in the Si IIλ6355, with this dropping to around one third in the six days before maximum light. We observed no difference between the populations of SNe Ia that do and do not form Si IIλ6355 HVFs in terms of the SALT2 light curve parameter x1, peak magnitude, decline rate, host mass, or host colour, supporting the idea that these features are ubiquitous across the SN Ia population.