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M96’s lopsided spiral arms and uneven gas and dust suggest that nearby galaxies have influenced it. But deep observations do not show clear evidence that M96 underwent a recent major merger. The evidence instead points to subtler interactions and possible gas accretion, while leaving the origin of the nearby Leo Ring unresolved.
Why does M96 look asymmetric?
M96, also catalogued as NGC 3368, is a spiral galaxy in the constellation Leo, about 35 million light-years away. NASA describes it as roughly comparable in mass and size to the Milky Way, with weak spiral arms, unevenly distributed gas and dust, and a core offset from the galaxy’s center. Its arms are also asymmetric; NASA says gravitational pull from other galaxies in the group is thought to have influenced them. That is a plausible interpretation of the galaxy’s appearance, not proof of a particular collision.
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M96 belongs to the M96 Group, also called the Leo I Group, which includes M95, M105, NGC 3384, and smaller galaxies. A galaxy’s shape can preserve signs of gravitational influence, but reconstructing a specific event requires weighing different kinds of evidence, including faint stars, gas, and the structures of neighboring galaxies.
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In a 2014 study, Watkins, Mihos, Harding, and Feldmeier searched deep, wide-field images for diffuse light in the group. They reported three extremely faint, streamlike features, with B-band surface brightnesses of approximately 29.2–29.9 magnitudes per square arcsecond. Such streams may be tidal features, and two may be associated with the Leo HI Ring. Their possible connection is an interpretation, not an established origin story.
The same study found no diffuse, large-scale optical counterpart to the extended HI ring down to its reported limits: μB = 30.1 and μV = 29.5 magnitudes per square arcsecond. Those limits describe the sensitivity of that study’s search; they do not mean the ring contains no stars or that no fainter optical signal could exist.
For M96 itself, the researchers found mild asymmetry in the extreme outer disk. They also observed color asymmetry that may reflect mild star formation associated with gas accretion from the HI ring. This is evidence consistent with gas accretion, not a direct demonstration of exactly how the gas arrived or what event formed the ring.
Is there evidence of a merger in the M96 Group?
The evidence varies from one galaxy to another, so features found elsewhere in the group should not be attributed to M96:
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| Galaxy or structure | Observed evidence | What it supports |
|---|---|---|
| M96 (NGC 3368) | Mild asymmetry in the extreme outer stellar disk; color asymmetry | Color differences may be associated with mild star formation and gas accretion from the HI ring. The observations do not establish a recent major merger. |
| NGC 3384 | Diffuse shells | The study interprets these as evidence consistent with a recent minor merger. |
| M105 and M95 | Outer isophotes appear almost undisturbed | The study found little sign of strong disturbance in their outer stellar structures. |
| Leo HI Ring | Extended neutral-hydrogen structure, with no diffuse, large-scale optical counterpart detected to the study’s stated limits | Its origin and its connection to individual group galaxies remain uncertain. |
Watkins and colleagues described interaction signatures across the group as “extremely subtle” for a group environment. They also noted tension between those subtle signatures and scenarios that require strong encounters to form the Leo HI Ring. The comparison matters: dramatic evidence of a minor merger in NGC 3384 does not show that M96 experienced the same event.
Independent reader supportYour contribution helps us test, update, and keep practical guides available for everyone.Did M96 collide with another galaxy?
The available observations do not establish a recent major collision involving M96. Its asymmetric arms and uneven gas distribution are consistent with gravitational influence from neighboring galaxies, and its outer-disk and color asymmetries are consistent with comparatively mild disturbance and possible gas accretion. But neither the galaxy’s appearance nor the faint streams provides a definitive reconstruction of a major merger.
Deep imaging also adds an important qualification: although it reveals very faint structures around the group, M96’s outer stellar disk remains only mildly asymmetric in the study’s account. Shallow views can miss diffuse features, but the deeper observations still do not show the kind of strong outer-disk disturbance that would settle the case for a recent, violent merger.
What is the Leo Ring, and is M96 pulling gas from it?
The Leo Ring is an extended structure of neutral hydrogen, or HI, in the M96 Group. The study found photometric evidence consistent with M96 accreting gas from it, including color asymmetry that may be linked to mild star formation. The evidence does not establish that M96 created the ring, that the ring came from a specific collision, or that the apparent connection to the faint streams is certain.
The ring’s origin remains an open question precisely because the group’s visible interaction signatures are subtle. The data support a possible relationship between M96 and the ring’s gas, while leaving the larger history unresolved.
Quick Recap
Sources and image identification
- NASA Science, “Hubble Peers into the Heart of a Galactic Maelstrom” (published September 4, 2015; updated March 28, 2025), for M96’s appearance, distance, and likely gravitational influence from group members.
- Watkins, Mihos, Harding, and Feldmeier, “Searching for diffuse light in the M96 Group” (first posted June 26, 2014), for the deep-imaging results and interpretations.
- ESA/Hubble, “A galactic maelstrom”, for the M96 image and object identification.
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