They have
strong hydrogen lines, at a maximum by A0, and also lines of ionized metals (Fe II, Mg II, Si II) at a maximum at A5.
Not exact matches
But the spectra from SN 2009ip show
strong lines of
hydrogen.
Indeed, its Lyman - alpha spectrum, i.e. one of the spectral
lines of
hydrogen it emits, is much narrower and
stronger than that of most galaxies, therefore confirming her theoretical predictions.
The 1992 supernova is known to have been one of these because
strong lines of
hydrogen appeared in its spectrum.
Type Ib and Ic supernovae result from the collapse of a massive star's core whose outer
hydrogen layers have been transfered to a companion star or blown off from
strong winds which is why they do not show
hydrogen emission
lines.
Type I supernovae happen in close binary systems and do not show
strong hydrogen emission
lines.
Type II supernovae happen in single star systems (or at least far enough away from any companion star to retain their
hydrogen outer layers) and have
strong hydrogen emission
lines.
Using Keck Observatory's powerful infrared spectrograph called MOSFIRE, the team dated the galaxy by detecting its Lyman - alpha emission
line — a signature of hot
hydrogen gas heated by
strong ultraviolet emission from newly born stars.
SDSS Collaboration Larger illustration Spectra of J1030 and another remote quasar displayed unexpectedly
strong lines of heavier elements, i.e., carbon, oxygen, nitrogen, and silicon (more on the «Gunn - Peterson trough» and the ionization of neutral
hydrogen).
Based on the extreme, deduced photometric redshift of GRB 000131 indicating that the gamma rays had travelled an extreme long cosmological distance, astronomers predicted a «break» in the red region of the spectrum around 670 to 700 nm from the
strong absorption of light from intervening intergalactic
hydrogen clouds along the
line of sight between GRB 000131 and the Solar System.