The New Galaxy: Signatures of Its Formation

By Kenneth C. Freeman, Joss Bland-Hawthorn. 2002

868 citations recorded by the source corpus.

▪ Abstract The formation and evolution of galaxies is one of the great outstanding problems of astrophysics. Within the broad context of hierachical structure formation, we have only a crude picture of how galaxies like our own came into existence. A detailed physical picture where individual stellar populations can be associated with (tagged to) elements of the protocloud is far beyond our current understanding. Important clues have begun to emerge from both the Galaxy (near-field cosmology) and the high redshift universe (far-field cosmology). Here we focus on the fossil evidence provided by the Galaxy. Detailed studies of the Galaxy lie at the core of understanding the complex processes involved in baryon dissipation. This is a necessary first step toward achieving a successful theory of galaxy formation.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/af0f032bb3e0566abba78e234502c4bef181938e

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Citations in the corpus

PLATO as it is: a legacy mission for Galactic archaeology (2017, neutral): “…abundance determinations that are key to inferring precise stellar properties (in particular age), to test stellar models, and, notably, for informing models of Galactic chemical evolution and to help identify populations of stars with a common origin (e.g., see Freeman & Bland-Hawthorn 2002).”
Thin, thick and dark discs in ΛCDM (2008, background): “(Freeman & Bland-Hawthorn 2002), as summarized in Table 1.”
The chemical compositions of Galactic disc F and G dwarfs (2002, background): “Freeman & Bland-Hawthorn (2002) refer to the resulting thick disc as a “ snap frozen ” relic of the state of the (heated) early disc.”
From Rings to Bulges: Evidence for Rapid Secular Galaxy Evolution at z ~ 2 from Integral Field Spectroscopy in the SINS Survey (2008, background): “It is tempting to speculate that the thick, old stellar disks seen in the Milky Way and nearby galaxies (e.g., Freeman & Bland-Hawthorn 2002; Yoachim & Dalcanton 2006) are the remnants of this z 2Y3 phase of transient evolution of clumpy, turbulent disks fed by rapid cold flows.”
Using chemical tagging to redefine the interface of the Galactic disc and halo (2015, background): “These components form the basis of any attempt to model, to simulate and to understand the formation and evolution of our Galaxy (see e.g. the reviews of Freeman & Bland-Hawthorn 2002; Ivezić, Beers & Jurić 2012, and references therein).”
THE LONG-TERM EVOLUTION OF THE GALACTIC DISK TRACED BY DISSOLVING STAR CLUSTERS (2010, methodology): “The technique of “chemical tagging” (Freeman & Bland-Hawthorn 2002) is being addressed by ongoing and planned stellar surveys.”
The Milky Way Tomography with SDSS. II. Stellar Metallicity (2008, background): “The three presumably discrete Milky Way components differ not only in their spatial profiles, but also in the detailed distributions of their kinematics and metallicity (e.g., Majewski 1993; Ojha et al. 1996; Freeman & Bland-Hawthorn 2002; Robin et al. 2003; Wyse 2006; and references therein).”
The Galaxy and its stellar halo: insights on their formation from a hybrid cosmological approach (2008, background): “It is interesting that in some cases there is a clear difference between the mean metallicity of stars in a given satellite (pockets of stars of different colours) - which is the basis of the ‘chemical tagging’ argument discussed in Freeman & Bland-Hawthorn (2002).”
The GALAH survey: observational overview and Gaia DR1 companion (2016, background): “Our overall science goal is to carry out chemical tagging (e.g., Freeman & Bland-Hawthorn 2002; De Silva et al. 2006; Bland-Hawthorn et al. 2010b) within this data set, identifying stars that formed at the same time and place by matching their abundance patterns.”
On the estimation of the local dark matter density using the rotation curve of the Milky Way (2019, neutral): “[10, 11]).”
Radial migration in disc galaxies — I. Transient spiral structure and dynamics (2011, background): “In the coming years, spectroscopic surveys, such as HERMES (Freeman & Bland-Hawthorn 2008) and APOGEE (Prieto et al. 2008), will obtain high-resolution spectroscopy of millions of stars, allowing finally for “chemical tagging” of stars into their birth clusters (Freeman & Bland-Hawthorn 2002).”
CHEMICAL EVOLUTION IN HIERARCHICAL MODELS OF COSMIC STRUCTURE. II. THE FORMATION OF THE MILKY WAY STELLAR HALO AND THE DISTRIBUTION OF THE OLDEST STARS (2009, background): “On the other hand, chemical abundances in the most metal-poor stars may preserve a record of early chemical evolution dating all the way back to the first stars (Freeman & Bland-Hawthorn 2002; Beers & Christlieb 2005).”
Stellar population gradients in galaxy discs from the CALIFA survey - The influence of bars (2014, background): “Spatially resolved stellar population studies in the disc region of spiral galaxies are sparse, with the exception of our own galaxy (see Freeman & Bland-Hawthorn 2002, for a review; Tables 1–3 and Appendices are available in electronic form at http://www.aanda.org Friel et al. 2002; Yong et al.…”
METALLICITY EVOLUTION OF DAMPED Lyα SYSTEMS OUT TO z ∼ 5 (2012, methodology): “We compare the stars to DLAs withz> 2, as the majority of the halo stars are believed to have formed by then (Freeman & Bland-Hawthorn 2002; Bullock & Johnston 2005; Robertson et al. 2005; Johnston et al. 2008).”
Evidence for an Intermediate-mass Milky Way from Gaia DR2 Halo Globular Cluster Motions (2018, background): “…distribution (or shape) are intrinsically linked to the formation and growth of structure in the Universe (Conselice 2014), so accurately determining these parameters for the MW will give us a clearer understanding of where our Galaxy sits in a cosmological context (Freeman & Bland-Hawthorn 2002).”
The GALAH survey and Gaia DR2: dissecting the stellar disc’s phase space by age, action, chemistry, and location (2018, background): “…U niversity user on 10 O ctober 2019 (Steinmetz et al. 2006), APOGEE (Majewski et al. 2017), GaiaESO (Gilmore et al. 2012), LAMOST (Deng et al. 2012) – and are now able to exploit the overlap of targets with Gaia DR2 – this is the golden age of Galactic archaeology (Freeman & Bland-Hawthorn 2002).”
Evidence from the H3 Survey That the Stellar Halo Is Entirely Comprised of Substructure (2020, background): “Further, stars belonging to the same structure share similar chemical abundance patterns (e.g., Freeman & Bland-Hawthorn 2002; Venn et al. 2004; Lee et al. 2015).”