To celebrate a new year, the NASA/ESA Hubble Space Telescope has published a montage of six beautiful galaxy mergers. Each of these merging systems was studied as part of the recent HiPEEC survey to investigate the rate of new star formation within such systems. These interactions are a key aspect of galaxy evolution and are among the most spectacular events in the lifetime of a galaxy.
It is during rare merging events that galaxies undergo dramatic changes in their appearance and in their stellar content. These systems are excellent laboratories to trace the formation of star clusters under extreme physical conditions.
The Milky Way typically forms star clusters with masses that are 10 thousand times the mass of our Sun. This doesn’t compare to the masses of the star clusters forming in colliding galaxies, which can reach millions of times the mass of our Sun.
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These dense stellar systems are also very luminous. Even after the collision, when the resulting galactic system begins to fade into a more quiescent phase, these very massive star clusters will shine throughout their host galaxy, as long-lasting witnesses of past merging events.
By studying the six galaxy mergers shown here, the Hubble imaging Probe of Extreme Environments and Clusters (HiPEEC) survey has investigated how star clusters are affected during collisions by the rapid changes that drastically increase the rate at which new stars are formed in these galaxies.
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- This image of NGC 3256 was taken with the Wide Field Camera 3 (WFC3) and the Advanced Camera for Surveys (ACS), both installed on the NASA/ESA Hubble Space Telescope. The galaxy is about 100 million light-years from Earth and provides an ideal target in which to investigate starbursts that have been triggered by galaxy mergers. Credit: ESA/Hubble, NASA
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- The galaxy system NGC 1614 has a bright optical centre and two clear inner spiral arms that are fairly symmetrical. It also has a spectacular outer structure that consists principally of a large one-sided curved extension of one of these arms to the lower right, and a long, almost straight tail that emerges from the nucleus and crosses the extended arm to the upper right. Credit: NASA, ESA, the Hubble Heritage Team (STScI/AURA)-ESA/Hubble Collaboration and A. Evans (University of Virginia, Charlottesville/NRAO/Stony Brook University)
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- NGC 4194 is also known as the Medusa merger. An early galaxy consumed a smaller gas-rich system, throwing out streams of stars and dust out into space. These streams, seen rising from the top of the merger galaxy, resemble the writhing snakes that Medusa, a monster in ancient Greek mythology, famously had on her head in place of hair, lending the object its intriguing name. The Medusa merger is located about 130 million light-years away in the constellation of Ursa Major (The Great Bear). Credit: ESA/Hubble & NASA, A. Adamo
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- This system consists of a pair of galaxies, dubbed IC 694 and NGC 3690, which made a close pass some 700 million years ago. As a result of this interaction, the system underwent a fierce burst of star formation. In the last fifteen years or so six supernovae have popped off in the outer reaches of the galaxy, making this system a distinguished supernova factory. Credit: NASA, ESA, the Hubble Heritage Team (STScI/AURA)-ESA/Hubble Collaboration and A. Evans (University of Virginia, Charlottesville/NRAO/Stony Brook University)
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- Located in the constellation of Hercules, about 230 million light-years away, NGC 6052 is a pair of colliding galaxies. They were first discovered in 1784 by William Herschel and were originally classified as a single irregular galaxy because of their odd shape. However, we now know that NGC 6052 actually consists of two galaxies that are in the process of colliding. This particular image of NGC 6052 was taken using Hubble’s Wide Field Camera 3. Credit: ESA/Hubble & NASA, A. Adamo et al.
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- Lying in the constellation Cetus (The Sea Monster), NGC 34’s outer region appears almost translucent, pin pricked with stars and strange wispy tendrils. This image shows the galaxy’s bright centre, a result of this merging event that has created a burst of new star formation and lit up the surrounding gas. As the galaxies continue to intertwine and become one, NGC 34’s shape will become more like that of a peculiar galaxy, devoid of any distinct shape. Credit: ESA/Hubble & NASA, A. Adamo et al.
Hubble’s capabilities have made it possible to resolve large star-forming “knots” into numerous compact young star clusters. Hubble’s ultraviolet and near-infrared observations of these systems have been used to derive star cluster ages, masses, and extinctions and to analyze the star formation rate within these six merging galaxies.
The HiPEEC study reveals that the star cluster populations undergo large and rapid variations in their properties, with the most massive clusters formed towards the end of the merger phase.
Each of the merging systems shown here has been previously published by Hubble, as early as 2008 and as recently as October 2020. To celebrate its 18th anniversary in 2008, the Hubble Space Telescope released a collection of 59 images of merging galaxies, which can be explored here.
More information
Reference: “Star cluster formation in the most extreme environments: insights from the HiPEEC survey” by A Adamo, K Hollyhead, M Messa, J E Ryon, V Bajaj, A Runnholm, S Aalto, D Calzetti, J S Gallagher, M J Hayes, J M D Kruijssen, S König, S S Larsen, J Melinder, E Sabbi, L J Smith and G Östlin, 3 September 2020, Monthly Notices of the Royal Astronomical Society.
DOI: 10.1093/mnras/staa2380
The Hubble Space Telescope is a project of international cooperation between ESA and NASA.
The HiPEEC survey was completed as part of the Hubble Space Telescope program GO 14066 (PI: A. Adamo). A repository with the study’s final data and catalogs is available here in the MAST Archive.
The international team of astronomers in this study consists of A. Adamo, K. Hollyhead, M. Messa, J. E. Ryon, V. Bajaj, A. Runholm, A. Aalto, D. Calzeti, J. S. Gallagher, M. J. Hayes, J. M. D. Kruijssen, S. König, S. S. Larsen, J. Melinder, E. Sabbi, L. J. Smith, and G. Östlin.
Source: SciTechDaily
