The Dynamics of Star Formation in Galaxies
Examining how different galaxies form stars and what influences the process.
Bryanne McDonough, Olivia Curtis, Tereasa Brainerd
― 4 min read
Table of Contents
Star formation in galaxies is a fascinating topic in the field of astronomy. Scientists are interested in how stars are born and how they grow in different types of galaxies. This study looks at a specific set of galaxies from a large simulation called TNG100, to see how a galaxy's characteristics affect its star formation.
Galaxy Types
Galaxies can be divided into two main types: central and satellite galaxies. Central galaxies are the big shots in their neighborhood. They sit at the heart of their group. Satellite galaxies, on the other hand, are like the sidekicks. They orbit around central galaxies and can be influenced by them. Understanding how these different types behave is crucial for learning more about star formation.
Key Factors Influencing Star Formation
Several factors can influence how and where stars form in galaxies. Here are the main players:
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Mass Of The Black Hole: Most central galaxies have supermassive black holes at their center. These black holes can affect the gas around them and play a role in star formation.
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Galaxy Shape: The physical form of a galaxy, whether it's a smooth round bulge or a stretched-out disk, can influence how stars form within it.
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Environment: A galaxy's surroundings, like whether it's in a crowded area with lots of other galaxies or a more isolated spot, can also have an impact.
Methods of Study
To study these effects, the researchers used something called radial profiles, which essentially show how different properties change as you move away from the center of a galaxy. They looked specifically at:
- Age of Stars: This tells us how long stars have been forming.
- Star Formation Rates: A measure of how many new stars are being made.
By comparing different groups of galaxies, the researchers could figure out what factors were really making a difference.
Findings on Central Galaxies
When examining central galaxies, the study found that those with more massive black holes tended to have older star populations. In other words, if a black hole is big, it might have already gobbled up a lot of gas needed for star formation, leading to an older average age of stars.
Inside-Out Quenching
A term you might hear in galactic discussions is "inside-out quenching." This fancy phrase simply means that star formation stops in the center of a galaxy first before it stops in the outer regions. It's like how you finish the snacks in the middle of a party before moving on to the leftover chips on the edges!
Satellite Galaxies and Their Quenching
Satellite galaxies didn't behave like their central counterparts. Instead, their star formation was more prone to being snuffed out due to environmental factors. If they were in dense areas with a lot of other galaxies, they were more likely to lose their star-forming gas.
Environmental Effects
The environment plays a key role in star formation. If a galaxy is in a busy area filled with other galaxies, the gravitational pull and interactions can strip away gas needed for star formation. This is especially true for satellite galaxies, which can feel the pressure from their bigger neighbors.
The Role of Time
How long a satellite galaxy has stayed in its host galaxy’s area matters too. The longer a satellite is around, the more likely it is to undergo these quenching processes, which can halt star formation. Time can be a sneaky factor in galactic evolution!
Summary of Results
The researchers concluded that high-mass galaxies tended to stop forming stars from the center outwards due to the influence of their black holes, while low-mass satellite galaxies were more affected by their surroundings. This information helps us understand the complex dance of star formation in galaxies.
Conclusions
Studying how galaxies form stars is a bit like detective work. You have to piece together clues from different areas, traits, and Environments to see the full picture. In the end, both intrinsic factors like black hole mass and extrinsic factors like the local galaxy density affect the star formation processes. It’s a cosmic balancing act, and scientists are only beginning to understand how all the pieces fit together.
Future Directions
There's still much more to explore in the realm of galaxies and star formation. Future research will delve deeper into how various factors interact and the specific processes that lead to quenching. Who knows? We might discover even more mysteries hidden in the depths of space!
And just like the stars, our curiosity continues to shine bright.
Title: Intrinsic and Environmental Effects on the Distribution of Star Formation in TNG100 Galaxies
Abstract: We present radial profiles of luminosity-weighted age, $age_L$, and $\Delta \Sigma_{SFR}$ for various populations of high- and low- mass central and satellite galaxies in the TNG100 cosmological simulation. Using these profiles, we investigate the impact of intrinsic and environmental factors on the radial distribution of star formation. For both central galaxies and satellites, we investigate the effects of black hole mass, cumulative AGN feedback energy, morphology, halo mass, and local galaxy overdensity on the profiles. In addition, we investigate the dependence of radial profiles of the satellite galaxies as a function of the redshifts at which they joined their hosts, as well as the net change in star-forming gas mass since the satellites joined their host. We find that high-mass ($M_*>10^{10.5} M_{\odot}$) central and satellite galaxies show evidence of inside-out quenching driven by AGN feedback. Effects from environmental processes only become apparent in averaged profiles at extreme halo masses and local overdensities. We find that the dominant quenching process for low-mass galaxies ($M_*
Authors: Bryanne McDonough, Olivia Curtis, Tereasa Brainerd
Last Update: 2024-11-20 00:00:00
Language: English
Source URL: https://arxiv.org/abs/2411.13666
Source PDF: https://arxiv.org/pdf/2411.13666
Licence: https://creativecommons.org/licenses/by/4.0/
Changes: This summary was created with assistance from AI and may have inaccuracies. For accurate information, please refer to the original source documents linked here.
Thank you to arxiv for use of its open access interoperability.