On January 29, 2002, a supernova was discovered by Yoji Hirose in the outer arms of the face-on spiral galaxy M74. The supernova is a rare Type Ib/c with a spectrum similar to SN1988bw, the only supernova associated with a gamma ray burst (GRB). Theoretical models to account for a GRB-SN connection base themselves on the collapse of a very massive star. Hypernovae are believed to produce black holes.
Students are using the UMBC telescope to observe this object with the hope of better understanding the nature of the violent deaths of supermassive stars. Students are following the brightness of the supernova as it changes with time. SN2002ap could be the Rosetta Stone for explaining GRBs!
The supernova went off in the outer spiral arms of the M74. Star formation is most active in spiral arms. Supernovae mark the end of the life of massive stars. Massive stars are short-lived (the candle twice as bright burns half as long). Hence, here there is star formation there are supernova.
The red box outlines the field of view containing the supernova images by the UMBC telescope (see below).
The supernova was imaged using the UMBC telescope by Dr. Eric Tittley at its peak brightness on February 8, 2002. This 3-colour image shows how blue the supernova is, particularly compared with the star to the east (left). All the other objects in this image are foreground stars in our own galaxy.
Using the UMBC telescope, students are following the progress of the supernova as its brightness changes with time. Since Type Ib/c supernovae are so rare, it is important to collect precise data for this once-in-a-lifetime event. The change in brightness of the supernova with time is produced by a variety of physics ranging from cooling of the initially hot plasma to the decay of radioactive nuclei.
Click on the image to view a PostScript version.
The photometric data is available for use. Please acknowledge the Joint Center for Astrophysics, UMBC.