New light on faint stars – III. Galactic structure towards the South Pole and the Galactic thick disc

Gilmore, G.; Reid, Neil

doi:10.1093/mnras/202.4.1025

Cited by 939 publications

(908 citation statements)

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“…The formation of galactic thick discs has been an important topic ever since their discovery in external galaxies (Burstein 1979;Tsikoudi 1979) and in the Milky Way (Gilmore & Reid 1983). The large uncertainties in important observational constraints in the Milky Way, such as the agevelocity-metallicity relation, abundance gradients and their evolution, have led to different scenarios to be proposed for the formation of the Galactic thick disc.…”

Section: The Galactic Thick Discmentioning

confidence: 99%

Constraining the Milky Way assembly history with Galactic Archaeology

Minchev

2016

Astron Nachr

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The aim of Galactic Archaeology is to recover the evolutionary history of the Milky Way from its present day kinematical and chemical state. Because stars move away from their birth sites, the current dynamical information alone is not sufficient for this task. The chemical composition of stellar atmospheres, on the other hand, is largely preserved over the stellar lifetime and, together with accurate ages, can be used to recover the birthplaces of stars currently found at the same Galactic radius. In addition to the availability of large stellar samples with accurate 6D kinematics and chemical abundance measurements, this requires detailed modeling with both dynamical and chemical evolution taken into account. An important first step is to understand the variety of dynamical processes that can take place in the Milky Way, including the perturbative effects of both internal (bar and spiral structure) and external (infalling satellites) agents. We discuss here (1) how to constrain the Galactic bar, spiral structure, and merging satellites by their effect on the local and global disc phase-space, (2) the effect of multiple patterns on the disc dynamics, and (3) the importance of radial migration and merger perturbations for the formation of the Galactic thick disc. Finally, we discuss the construction of Milky Way chemo-dynamical models and relate to observations.

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Section: The Galactic Thick Discmentioning

confidence: 99%

Constraining the Milky Way assembly history with Galactic Archaeology

Minchev

2016

Astron Nachr

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“…With the availability of sensitive emulsions, automated measuring machines, and sophisticated computers, large photographic color surveys have been carried out over large areas of the sky at high galactic latitude (where contamination by red giants and heavilyreddened background stars is not a problem). Gilmore and Reid (1983) presented the first large samples, as did Hawkins (1986) and his collaborators. Still, the surface area of the sky covered by the color surveys does not yet approach that of the Luyten proper motion surveys.…”

Section: Optical and Infrared Color Surveysmentioning

confidence: 94%

Searches for Brown Dwarfs

Liebert

1994

International Astronomical Union Colloquium

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“…The thin disk is embedded in a lower-density, kinematically hotter stellar population consisting of older, more metal-poor stars -the thick disk (Gilmore & Reid 1983;Bensby et al 2005). The chemical similarity of Galactic bulge and thick disk stars might suggest that the Milky Way does not have a classical bulge (Meléndez et al 2008).…”

Section: Disks and Long-term Evolutionary Trends For Disk Galaxiesmentioning

confidence: 99%

Observational Comparison of Star Formation in Different Galaxy Types

Grebel

2010

Proc. IAU

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Abstract. Galaxies cover a wide range of masses and star formation histories. In this review, I summarize some of the evolutionary key features of common galaxy types. At the high-mass end, very rapid, efficient early star formation is observed, accompanied by strong enrichment and later quiescence, well-described by downsizing scenarios. In the intermediate-mass regime, early-type galaxies may still show activity in low-mass environments or when being rejuvenated by wet mergers. In late-type galaxies, we find continuous, though variable star formation over a Hubble time. In the dwarf regime, a wide range of properties from bursty activity to quiescence is observed. Generally, stochasticity dominates here, and star formation rates and efficiencies tend to be low. Morphological types and their star formation properties correlate with environment.

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New light on faint stars – III. Galactic structure towards the South Pole and the Galactic thick disc

Cited by 939 publications

References 0 publications

Constraining the Milky Way assembly history with Galactic Archaeology

Constraining the Milky Way assembly history with Galactic Archaeology

Searches for Brown Dwarfs

Observational Comparison of Star Formation in Different Galaxy Types

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