Facts about Messier 109
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A small group of at least three satellite galaxies orbit Messier 109, making it a gravitationally dominant system within its local region of the Ursa Major cluster.
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Dust lanes in Messier 109 show a striking asymmetry between its leading and trailing spiral arms, indicating ongoing dust redistribution from the bar's gravitational torques.
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Messier 109's central supermassive black hole has an estimated mass of approximately 40 million solar masses, making it significantly more massive than most barred spiral galaxies of comparable size.
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Messier 109's disk exhibits a measurable inclination of approximately 68 degrees relative to our line of sight, making it one of the more obliquely oriented major galaxies in the Ursa Major cluster.
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Active star formation in Messier 109 occurs primarily within its bar region, where gas densities are elevated by the dynamics of the rotating bar structure.
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The outer spiral arms of Messier 109 show a warped structure, likely caused by gravitational interactions with nearby galaxies in the Ursa Major cluster.
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Messier 109's prominent bar structure rotates at a different angular velocity than its disk, a characteristic observed in many barred spirals that influences star formation patterns.
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NGC 3992, the technical designation for Messier 109, was discovered by Pierre Méchain in 1781 during his systematic survey of the northern sky.
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Approximately 83 million light-years away, Messier 109 is a barred spiral galaxy in the constellation Ursa Major containing roughly 100 billion stars.