The luminous and rapidly evolving SN 2018bcc - Clues toward the origin of Type Ibn SNe from the Zwicky Transient Facility

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Volume 649 (May 2021)

A&A, 649 (2021) A163

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Table C.2.

FWHM and P-Cygni absorption velocities inferred from fitting different lines present at t > +14 d.

Line	P-Cygni maximum absorption	Terminal velocity (BVZI)	FWHM
(Å)	(km s⁻¹)	(km s⁻¹)	(km s⁻¹)
He I 3889	925, 953, 1350	1914, 1830, 1618	1830, 1860, 1040 ^(a)
He I 4471 ^(b)	800, 845, 1174	1550, 1750, 1850	1020, 1380, 1790 ^(a)
He I 4922 ^(c)	834, 1087, –	1400, 1590, –	1107 ^(a), 704, 2920 ^(a)
He I 5016 ^(d)	1157, 1221, –	1745, 1954, –	755 , 721, 2600 ^(a)
He I 5876	1000, 1020, –	1600, 1356, –	3000, 3020, 3000
He I 6678	990, 1070, –	1470, 1428, –	1950, 2080, 1650
He I 7065	1060, – , –	1645, – , –	2520, 2100, 1871 ^(a)

Notes.

Velocities are spaced with a comma and refer to the fits made on the +14 d, +20 d and +52 d spectrum (P200, first and second Keck spectrum), respectively and refer to the atomic line reported in the first column. Systematic redshift uncertainty of ∼300 km s⁻¹ applies while typical measurement uncertainties are ∼200–300 km s⁻¹ based on noise.

^(a)

Uncertain measurements due to the lower S/N of the spectrum at those wavelengths

^(b)

Possibly contaminated by Mg IIλ 4481 line.

^(c)

Possibly contaminated by Fe IIλ 4924 line.

^(d)

Possibly contaminated by He Iλ 5048 and Fe IIλ 5018 lines.

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