EVOLUTION OF THE STARS AND GAS IN GALAXIES.

By B. Tinsley. 2022

284 citations recorded by the source corpus.

Essentially everything of astronomical interest is either part of a galaxy, or from a galaxy, or otherwise relevant to the origin or evolution of galaxies. Diverse examples are that the isotropic composition of meteorites provides clues to the history of star formation billions of years ago, and cosmological tests for the deceleration of the Universe are strongly affected by changes in the luminosities of galaxies during the lookback time sampled. The aim of this article is to review some of the vital connections that galaxy evolution makes among many astronomical phenomena. The evolution of galaxies can be broadly divided into three areas: dynamical evolution, chemical evolution, and the evolution of photometric properties. Chemical and photometric evolution are the main topics of this review, and dynamical processes will be considered only where they directly affect the others. The article is intended to be self-contained for readers with a general knowledge of astronomy and astrophysics but with no special expertise on galaxies. Because the background and literature relevant to the evolution of stars and gas in galaxies are so extensive, complete coverage cannot be attempted. Instead, comprehensive reviews and recent papers are emphasized in the references; these include detailed works in closely related fields, such as galaxy formation and nucleosynthesis, that are treated very briefly here. The history of the subject has been discussed in several recent reviews (e.g. Sandage et al. 1975; Spinrad & Peimbert 1975; Trimble 1975; van den Bergh 1975), so here the emphasis will be on current ideas.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

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Citations in the corpus

The SAURON project – VII. Integral-field absorption and emission-line kinematics of 24 spiral galaxy bulges (2006, background): “Since the first estimates of SFRs using colours (e.g. Tinsley 1968), many different diagnostics have been proposed to measure the amount of stellar mass produced in a given time [i.e. ultraviolet continuum, recombination lines, forbidden lines, far-infrared continuum; see Kennicutt (1998) for an…”
DWARF GALAXY STARBURST STATISTICS IN THE LOCAL VOLUME (2008, methodology): “…evolution studies uses the present-day integrated properties of galaxies, in particular the UBV colors and Hα-based SFRs, to infer the SFHs (e.g., Tinsley 1968, 1972; Searle et al. 1973; Gallagher et al. 1984; Kennicutt 1998 and references therein; van Zee 2001; Bruzual & Charlot 2003 and…”
The Galaxy Evolution Explorer: A Space Ultraviolet Survey Mission (2004, background): “Tinsley, in her seminal 1968 paper (Tinsley 1968), demonstrated that passive stellar evolution and an evolving stellar birthrate required to match the properties of nearby galaxies had a profound impact on the appearance of galaxies observed over cosmological distances.”
Oxygen abundances in nearby stars - Clues to the formation and evolution of the Galactic disk (2007, unknown): “The steep decline in the thin disk [O/Fe] ratio indicates that the chemical enrichment of the ISM was due to both SN Ia and SN II, as proposed originally by Tinsley (1980), and demonstrated here, in Fig.”
Origin of the heaviest elements: The rapid neutron-capture process (2019, background): “and outflow of enriched material out of the Galaxy (for a review of early investigations see e.g. Audouze and Tinsley, 1976; Tinsley, 1980).”
De re metallica: the cosmic chemical evolution of galaxies (2018, background): “When the infall is halted, the galaxy evolves as a closed box (Searle & Sargent, 1972; Tinsley, 1980), reducing gas fraction, enriching gas with the residual, decreasing activity of star formation, and producing stars with rapidly increasing metallicities, primarily as a consequence of the lack of…”
A Binary Model for the UV-upturn of Elliptical Galaxies (2006, methodology): “The technique was first devised by Tinsley (Tinsley 1968) and has experienced rapid development ever since (Bruzual & Charlot 1993; Bressan et al. 1994; Worthey 1994; Tantalo et al. 1996; Zhang et al. 2002; Bruzual & Charlot 2003; Zhang et al. 2004a).”
The UV-Optical Galaxy Color-Magnitude Diagram. III. Constraints on Evolution from the Blue to the Red Sequence (2007, unknown): “In this case we assume that galaxies were formed 10 Gyr ago with a range of e-folding parameters that accounts for the range in present day colors, the original assumption of Tinsley (1968).”
Production of dust by massive stars at high redshift (2011, background): “For a profoundreview on chemical evolution models see Tinsley (1980), Dwek (1998), Dwek et al (2009) or Pi van et al (2011a,b).”
The Evolving Luminosity Function of Red Galaxies (2006, background): “The stellar populations of these galaxies are dominated by an old component, with little ongoing star formation (e.g., Tinsley 1968).”
Galaxy morphology and star formation in the Illustris Simulation at z = 0 (2015, methodology): “The principal idea is to apply stellar population synthesis techniques (e.g., Tinsley 1968; Tinsley & Gunn 1976; Tinsley & Larson 1978; Gunn et al. 1981) to galaxy evolution models.”
[O II] as a Star Formation Rate Indicator (2004, background): “The star formation rate indicators developed four decades ago provided a first quantitative measure of the global star formation in galaxies (Tinsley 1968, 1972; Searle, Sargent, & Bagnuolo 1973).”
Dynamics for galactic archaeology (2013, background): “…the chemical evolution of galaxies modelled the annulus of gas within the Galaxy with R ∼ R0 as a box that initially contained just pristine gas but gradually contained more and more stars and more highly enriched gas (van den Bergh, 1962; Schmidt, 1963; Tinsley, 1968; Pagel & Patchett, 1974).”
AN ATLAS OF GALAXY SPECTRAL ENERGY DISTRIBUTIONS FROM THE ULTRAVIOLET TO THE MID-INFRARED (2013, methodology): “Galaxy SEDs can be modeled using models of stel- lar populations, nebular emission lines, dust obscuration and dust emission (e.g., Tinsley 1968; Silva et al. 1998; Charlot & Longhetti 2001; Bruzual & Charlot 2003; Maraston 2005; da Cunha et al. 2008; Vega et al. 2008; Pacifici et al. 2012).”
Modeling the Panchromatic Spectral Energy Distributions of Galaxies (2013, methodology): “At about the same time, synthesis models were being developed that relied on stellar evolution theory to constrain the range of possible stellar types at a given age and metallicity (e.g., Tinsley 1968, Searle, Sargent & Bagnuolo 1973, Tinsley & Gunn 1976, Bruzual 1983).”
Evolutionary stellar population synthesis at high spectral resolution: optical wavelengths (2005, methodology): “Evolutionary synthesis, introduced by Tinsley (1968), is a powerful tool for interpreting the integrated light of a stellar population.”
The UV-Optical Color Magnitude Diagram. II. Physical Properties and Morphological Evolution On and Off of a Star-forming Sequence (2007, background): “This suggests that non-SF galaxies are not simply SF galaxies of the same stellar mass that have stopped forming stars—a result consistent with the observed correlation between SFH and structure.”
Galaxy Luminosity Functions to z~1 from DEEP2 and COMBO-17: Implications for Red Galaxy Formation (2005, background): “For example, it was known that early-type galaxies are more luminous and more massive than later-type galaxies (de Vaucouleurs 1977, Binggeli & Sandage 1985) and that their stellar populations are on average older (e.g., Tinsley 1968, Searle, Sargent & Bagnuolo 1973).”