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

By G. Gilmore, N. Reid. 1983

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Citations in the corpus

Yule-Simpson’s paradox in Galactic Archaeology (2019, background): “When the total stellar population is considered, the vertical disk density at all radii requires a sum of two exponentials for a proper fit (Gilmore & Reid 1983).”
Dissecting simulated disc galaxies - I. The structure of mono-age populations (2014, background): “The stellar disc of the Milky Way, as well as of many nearby galaxies, is traditionally viewed as consisting of two distinct components: a thin and a thick disc (e.g., Burstein 1979; Tsikoudi 1979; Gilmore & Reid 1983; Dalcanton & Bernstein 2002; Yoachim & Dalcanton 2006; Comerón et al. 2011).”
The mass distribution and gravitational potential of the Milky Way (2016, background): “The Milky Way’s stellar disc is commonly decomposed into a thin and thick disc (e.g.Gilmore & Reid 1983).”
Galactic stellar haloes in the CDM model (2009, background): “Observations of the Milky Way and analogous galaxies frequently distinguish a ‘thick disc’ component (Gilmore & Reid 1983; Carollo et al. 2010) thought to result either from dynamical heating of the thin disc by minor mergers (e.g. Toth & Ostriker 1992; Quinn, Hernquist & Fullagar 1993; Velazquez &…”
Measuring the vertical age structure of the Galactic disc using asteroseismology and SAGA (2015, background): “Star counts have revealed that the disc of the Milky Way is best described by two populations, one with shorter and one with longer scaleheights, dubbed the ‘thin’ and the ‘thick’ disc (e.g. Gilmore & Reid 1983; Jurić et al. 2008).”
THE METALLICITY DISTRIBUTION FUNCTIONS OF SEGUE G AND K DWARFS: CONSTRAINTS FOR DISK CHEMICAL EVOLUTION AND FORMATION (2011, background): “Gilmore & Reid (1983) first detected the thick disk in the Milky Way when they determined that the stellar number density as a function of height above the plane was best fit by two components,18 one with a scale height of approximately 300 pc, and the second with a scale height of 1350 pc.…”
Nearby stars of the Galactic disc and halo – IV (2008, unknown): “The latter immediately manifest that both populations are disc-like, albeit on different scaleheights, and hence the terms ‘thick disc’ and ‘thin disc’ as originally introduced in the landmark research by Gilmore & Reid (1983).”
TRACING CHEMICAL EVOLUTION OVER THE EXTENT OF THE MILKY WAY'S DISK WITH APOGEE RED CLUMP STARS (2014, background): “Various qualitatively different scenarios for the formation of the thick, old, high-α component in the MW have been suggested since the result was first identified by Yoshii (1982) and Gilmore & Reid (1983).”
Oxygen abundances in nearby stars - Clues to the formation and evolution of the Galactic disk (2007, background): “Using star counts, Gilmore & Reid (1983) were the first to provide compelling evidence for the existence of the Galactic thick disk.”
The Lives of Stars: Insights from the TGAS–RAVE–LAMOST Data Set (2018, background): “…therein) and is useful for exploring differences between spatially mixed populations, such as those of the canonical thin and thick disks (Gilmore & Reid 1983), which are thought to have different formation histories and thus chemistry (see Fuhrmann 1998, and later Bovy et al. 2012 and…”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, background): “The Milky Way seems to have a two-component disc as well, which was first proposed to fit the vertical density profile derived from star counts (Yoshii 1982; Gilmore & Reid 1983).”
Massive runaway and walkaway stars (2018, background): “For comparison, the typical size of OBassociations is on the order of tens of pc, while the Galactic thin and thick disks have a vertical scale height of∼300 and∼1500 pc, respectively (e.g., Gilmore & Reid 1983).”
Impacts of a flaring star-forming disc and stellar radial mixing on the vertical metallicity gradient (2016, background): “Both the Milky Way (Yoshii 1982; Gilmore & Reid 1983) and external galaxies (e.g. Burstein 1979; Dalcanton & Bernstein 2002) show geometrically thick discs in addition to the geometrically thin disc.”
The New Galaxy: Signatures of Its Formation (2002, background): “The galactic thick disk was first recognized by Gilmore & Reid (1983).”
Star Counts Redivivus. IV. Density Laws through Photometric Parallaxes (2002, background): “Most studies have focused upon one or a few directions in the sky generally either in tiny areas to great depth (e.g., Paper I; Paper II) or over a large area to shallower depth (e.g., Gilmore & Reid 1983, hereafter GR83).”
The Milky Way Tomography with SDSS. I. Stellar Number Density Distribution (2005, methodology): “16 The use of photometric parallax to determine Galactic model parameters is not particularly novel, having a long history going back to at least Gilmore & Reid (1983).”
The Galaxy and its stellar halo: insights on their formation from a hybrid cosmological approach (2008, background): “A much smaller mass of stars (about 10-20 per cent of that in the thin disk) reside in a distinct component which was established about 25 years ago though star counts (Gilmore & Reid 1983), and which is referred to as the ‘thick disk’.”
The stellar halo of the Galaxy (2008, background): “They have led to the conclusion that our Galaxy has several physically distinct components, namely the thin and thick disk, the stellar halo and the bulge/bar (e.g. Bahcall & Soneira 1980; Gilmore & Reid 1983).”
THE GENESIS OF THE MILKY WAY'S THICK DISK VIA STELLAR MIGRATION (2010, methodology): “…to previous work (e.g. Bahcall & Soneira 1980) which identifies a clear change of slope in the counts of disk stars as a function of distance from the Galactic plane; this change in slope is usually interpreted as the transition from the thin to thick disk (Gilmore & Reid 1983; Siegel et al. 2002).”