| 12 Galaxies were actively forming and merging at high rates. |
| 12 Some of the first massive galaxies were already taking shape. |
| 12 These galaxies were often small and irregular, but some began forming spiral structures. |
| 12 The universe was entering a period called “cosmic noon” (which peaked around 10 billion years ago). |
| 12 This was a high point for star formation — new stars were being born at rates far greater than today. |
| 12 Many Population II stars were forming, which are metal-poor but not as ancient as Population III stars. |
| 12 Quasars — extremely bright and energetic centers of young galaxies powered by supermassive black holes — were common. |
| 12 Black holes in the centers of galaxies were rapidly growing by consuming matter. |
| 12 Supernovae from earlier generations of stars were enriching the interstellar medium with heavier elements like carbon, oxygen, and iron. |
| 12 These metals were beginning to influence the formation of planets and life-essential compounds. |
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| 11 - 8 The universe entered a phase known as "Cosmic Noon," the period of maximum star formation in galaxies. |
| 11 - 8 Galaxies were forming stars at rates much higher than they do today—up to 100 times faster. |
| 11 - 8 Massive galaxies were assembling and evolving rapidly, leading to the creation of many of the stars that still shine in galaxies like the Milky Way. |
| 11 Galaxies were merging frequently, leading to the formation of larger galaxies. |
| 11 These mergers triggered starbursts and built up the large spiral and elliptical galaxies we see today. |
| 11 Many of today’s giant elliptical galaxies likely formed during this time. |
| 11 Active galactic nuclei (AGN) were common; these are powered by rapidly growing supermassive black holes. |
| 11 Quasars—some of the most luminous objects in the universe—were abundant. |
| 11 Black holes at the centers of galaxies were consuming gas and emitting intense radiation. |
| 11 Early supernovae from massive stars began enriching the universe with heavier elements (carbon, oxygen, iron, etc.). |
| 11 These elements spread through space, seeding future stars, planets, and eventually life. |
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| 10 Population III stars, the very first generation of stars (massive and short-lived), had already exploded as supernovae by this point, enriching the universe with heavier elements (like carbon, oxygen, and iron) needed for future stars and planets. |
| 10 Population II stars were now common, and globular clusters were forming. |
| 10 However, elements essential for rocky planets (like silicon and iron) were being spread into the interstellar medium. |
| 10 Clusters of galaxies and cosmic filaments were becoming more defined due to gravitational attraction. |
| 10 Dark matter halos were helping galaxies gather mass and structure. |
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