The CfA team observed
SN 2017egm on June 18th with the 60 - inch telescope at the Smithsonian Astrophysical Observatory's Fred Lawrence Whipple Observatory in Arizona.
While the brightness of
SN 2017egm and the properties of the magnetar that powers it overlap with those of other superluminous supernovas, the amount of mass ejected by
SN 2017egm may be lower than the average event.
The CfA researchers also found more clues about the nature of
SN 2017egm.
Building on this discovery, the CfA team found that
SN 2017egm's host galaxy has a high concentration of elements heavier than hydrogen and helium, which astronomers call «metals.»
Also, the spin rate of
SN 2017egm's magnetar may be slower than usual.
SN 2017egm shares magnetar properties with other superluminous supernovas, but the researchers noted that the newly discovered supernova does have some differences.
The researchers also investigated what makes
SN 2017egm so bright.
For example,
SN 2017egm might have ejected less mass than its supernova counterparts because its massive star might have shed mass before exploding.
In fact,
SN 2017egm was not only superluminous, but superclose: At just 420 million light - years away, it was three times closer than any other observed supernova of its type.
New research zeroes in on one supernova, called
SN 2017egm, which exploded May 23 within view of the European Space Agency's Gaia satellite, which monitors star positions.