The galaxy has a morphological classification of SB(r)b,[1] with the SBb notation indicating it is a barred spiral with arms that are intermediate on the scale from tightly to loosely wound, and an "(r)" meaning an inner ring surrounds the bar.[4] The latter is a ring-shaped, circumnuclearstar-forming region with a diameter of approximately 70,000 light-years (21,000 pc).[5] The spiral structure extends outward from the ring.[4]
Its ring structure is about3.5×108M☉ (solar masses) in molecular gas and yields a star formation rate of 0.38 M☉ yr−1.[a] The star formation is occurring in at least five regions with diameters between 100 and 150 pc that are composed of several star clusters ranging in size from 1.7 to 4.9 pc. These individual clusters contain(1.8–8.7)×106M☉[b] of stars, and may be on the path to formingglobular clusters.[6]
SN 2012aw (TypeII-P, mag. 15) was discovered by Paolo Fagotti and independently by Jure Skvarc on 16 March 2012.[11][12][13][14] Thelight curve of this displayed great flattening after 27 days, thus classifying it as a Type II-P, or "plateau", core-collapse supernova.[15] The disappearance of the progenitor star was later confirmed from near-infrared imaging of the region. The brightness from the presumedred supergiant progenitor allowed its mass to be estimated as12.5±1.5 M☉.[16]
Optical and radio information are combined in this image of M95, showing the process of " stellar feedback", redistributing energy into the interstellar medium causing star-forming (blue area).[17]Image of M95 taken by James Webb'sMIRI andNIRCam instruments.
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