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Table 4.

Mass fractions of the different elements included in our sequence of best-fitting TARDIS models.

Element Mass fraction Velocity range (km s−1)
He 0.69 3500 − 18 000
O 0.30 3500 − 18 000
Ca 10−4 12 000 − 18 000
56Ni (a)(b) 0.01 3500 − 17 000
H (c) ≲0.04 3500 − 18 000
C < 0.05 3500 − 18 000
Na < 0.05 3500 − 18 000
Mg < 0.10 3500 − 18 000
Si < 0.05 3500 − 18 000
S (d) ≲0.5 3500 − 18 000

Notes. The mass fractions included apply only to the velocity ranges quoted (outside these ranges the mass fractions are set to zero, with any deviation from a mass fraction of unity compensated for by slightly increasing or decreasing the He mass fraction).

(a)

Our models included this initial mass fraction of 56Ni (at t = 0 days). Its mass fraction was updated at subsequent epochs, accounting for the effects of radioactive decay.

(b)

Our early model (at +0.9 days) cannot accommodate any significant quantity of 56Ni, and so this outermost region of the ejecta (vej = 17 000 − 18 000 km s−1) is free of IGEs across our sequence of spectra.

(c)

This is the mass fraction of H needed to reproduce the emission at ∼6600 Å, although we expect this to be somewhat uncertain, due to the limitations of our LTE approximations.

(d)

Our S mass fraction remained reasonably unconstrained across our sequence of models, as evidenced by the fact we can accommodate an unphysically large mass fraction.

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