Astrophysics II Unit 9 Review: Galaxy Formation and Evolution

Key Concepts and Theories

• Galaxies are vast cosmic structures composed of stars, gas, dust, and dark matter held together by gravity
• Hubble sequence classifies galaxies into three main types: elliptical, spiral, and irregular based on their morphology and structure
• Hierarchical structure formation suggests galaxies form through the merging and accretion of smaller structures over cosmic time
• Cold dark matter (CDM) model proposes that dark matter halos provide the gravitational framework for galaxy formation and evolution
• Baryon cycle describes the flow of gas into and out of galaxies, including processes such as accretion, star formation, and feedback
• Cosmic web refers to the large-scale structure of the universe, consisting of filaments, walls, and voids, with galaxies forming at the intersections
• Initial mass function (IMF) describes the distribution of stellar masses formed in a galaxy, which influences its overall properties and evolution
• Feedback mechanisms, such as supernovae and active galactic nuclei (AGN), regulate star formation and shape the interstellar medium (ISM) in galaxies

Galactic Building Blocks

• Gas is the primary raw material for galaxy formation, providing the fuel for star formation and the growth of galactic structures
• Dark matter halos serve as the gravitational scaffolding for galaxy formation, influencing the distribution and dynamics of baryonic matter
• Stars are the fundamental building blocks of galaxies, forming from collapsing clouds of gas and dust in the ISM
• Globular clusters are ancient, compact groups of stars that formed early in a galaxy's history and provide insights into its formation and evolution
• Dust grains play a crucial role in the ISM, absorbing and scattering light, and serving as sites for molecular formation and star formation
• Metals, elements heavier than helium, are produced by stellar nucleosynthesis and enrich the ISM, influencing the properties of subsequent generations of stars
• Supermassive black holes reside at the centers of most galaxies and can significantly impact their evolution through AGN feedback
• Satellite galaxies are smaller galaxies that orbit and interact with larger host galaxies, often being disrupted and merged over time

Galaxy Formation Models

• Monolithic collapse model proposes that galaxies formed early and rapidly from the collapse of massive gas clouds, with little subsequent evolution
• Hierarchical merging model suggests galaxies form through the gradual merging and accretion of smaller structures, with more massive galaxies forming later
• Press-Schechter formalism provides a statistical description of the abundance and mass distribution of dark matter halos as a function of redshift
• Semi-analytic models (SAMs) combine dark matter halo merger trees with analytic prescriptions for baryonic physics to simulate galaxy formation and evolution
• Hydrodynamical simulations incorporate gas dynamics and feedback processes to model galaxy formation and evolution in a more self-consistent manner
• Subhalo abundance matching (SHAM) connects the properties of galaxies to those of their host dark matter halos, assuming a monotonic relationship between stellar mass and halo mass
• Halo occupation distribution (HOD) describes the probability distribution of the number of galaxies residing in a dark matter halo of a given mass
• Conditional luminosity function (CLF) extends the HOD approach by considering the luminosity distribution of galaxies within halos

Evolution of Galaxy Structures

• Disk formation occurs as gas cools and settles into a rotating disk, supported by its angular momentum
• Bulge growth can result from various processes, including disk instabilities, mergers, and secular evolution
• Spiral arms are density waves in the disk, triggered by gravitational instabilities or tidal interactions, and are sites of enhanced star formation
• Bar formation is a common disk instability that redistributes angular momentum and drives gas inflow, potentially fueling central starbursts or AGN
• Galactic outflows, driven by stellar or AGN feedback, can remove gas from galaxies and regulate their star formation and chemical evolution
• Morphological transformations, such as the conversion of spirals into ellipticals through mergers, shape the galaxy population over cosmic time
• Environmental effects, such as ram-pressure stripping and harassment, can alter the structure and properties of galaxies in dense environments like clusters
• Stellar halos, composed of old, metal-poor stars, provide a fossil record of a galaxy's accretion history and early formation

Observational Techniques and Evidence

• Multi-wavelength observations, from radio to gamma rays, provide a comprehensive view of galaxy properties and evolution
• Redshift surveys map the 3D distribution of galaxies, revealing the large-scale structure of the universe and the cosmic web
• Hubble Deep Fields are long-exposure images that capture the most distant and faintest galaxies, providing insights into early galaxy formation and evolution
• Integral field spectroscopy (IFS) enables spatially resolved studies of galaxy kinematics, star formation, and chemical composition
• Gravitational lensing, the bending of light by massive structures, allows the detection and study of distant, otherwise unobservable galaxies
• Tully-Fisher relation correlates a spiral galaxy's luminosity with its rotation velocity, serving as a distance indicator and probe of dark matter content
• Fundamental plane relates the size, surface brightness, and velocity dispersion of elliptical galaxies, providing insights into their structure and evolution
• Galaxy scaling relations, such as the mass-metallicity and star formation rate-mass relations, reveal fundamental connections between galaxy properties and their evolutionary histories

Star Formation and Stellar Populations

• Star formation rate (SFR) quantifies the mass of stars formed per unit time in a galaxy, typically measured using tracers like UV, H-alpha, or infrared emission
• Kennicutt-Schmidt law relates the surface density of gas to the surface density of star formation, indicating that star formation is regulated by gas availability
• Stellar population synthesis models predict the integrated light of a galaxy based on its star formation history and initial mass function
• Color-magnitude diagram (CMD) plots the brightness and color of individual stars in a galaxy, revealing its star formation history and age distribution
• Main sequence of star-forming galaxies is a tight correlation between a galaxy's SFR and stellar mass, with more massive galaxies exhibiting higher SFRs
• Starburst galaxies experience intense episodes of star formation, often triggered by mergers or interactions, and can rapidly exhaust their gas supply
• Quenching refers to the suppression of star formation in galaxies, which can occur through various mechanisms such as gas depletion, feedback, or environmental effects
• Stellar feedback, including supernovae and stellar winds, can heat and expel gas from galaxies, regulating their star formation and shaping the ISM

Dark Matter and Galaxy Dynamics

• Rotation curves of spiral galaxies reveal flat velocity profiles at large radii, indicating the presence of dark matter halos
• Velocity dispersion of stars and gas in elliptical galaxies and galaxy clusters provides evidence for dark matter, as the observed motions exceed those expected from visible matter alone
• NFW profile is a commonly used model for the density distribution of dark matter halos, characterized by a cuspy inner profile and a steep outer slope
• Substructure refers to the presence of smaller, self-bound dark matter clumps within larger halos, which can host satellite galaxies and contribute to tidal disruption and merging
• Gravitational interactions between galaxies, such as tidal stripping and dynamical friction, can alter their orbits and lead to mergers and morphological transformations
• Missing satellites problem refers to the discrepancy between the predicted abundance of low-mass dark matter halos and the observed number of satellite galaxies around the Milky Way
• Dark matter annihilation or decay could potentially produce observable signals, such as gamma rays or X-rays, providing indirect evidence for the nature of dark matter
• Modified gravity theories, such as MOND (Modified Newtonian Dynamics), attempt to explain galaxy dynamics without invoking dark matter, but face challenges in reconciling with other cosmological observations

Current Research and Open Questions

• Reionization and the role of early galaxies in ionizing the neutral hydrogen in the universe during the first billion years remain active areas of research
• Feedback processes, particularly AGN feedback and its impact on galaxy evolution, are still not fully understood and are the subject of ongoing investigations
• Galactic winds and outflows, their driving mechanisms, and their influence on the CGM and IGM are topics of current research interest
• The nature of dark matter, whether it is cold, warm, or self-interacting, and its role in galaxy formation and evolution, remains an open question
• The origin and evolution of supermassive black holes, their co-evolution with host galaxies, and the impact of AGN feedback are active research areas
• The assembly history of the Milky Way and the properties of its stellar halo, satellite galaxies, and globular clusters are being investigated through large surveys and simulations
• The connection between galaxy properties and their environment, particularly in the context of galaxy clusters and the cosmic web, is an ongoing research topic
• The role of mergers and interactions in shaping galaxy morphologies, triggering starbursts, and fueling AGN activity is being studied through observations and simulations