Stellar Population Studies with the SDSS. I. The Vertical Distribution of Stars in the Milky Way

By Bingqiu Chen, C. Stoughton, J. A. Smith, A. Uomoto, J. Pier, Brian Yanny, Željko Ivezic´, D. York, John E. Anderson, James Annis and 7 more. 2001

297 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

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KINEMATICAL AND CHEMICAL VERTICAL STRUCTURE OF THE GALACTIC THICK DISK. II. A LACK OF DARK MATTER IN THE SOLAR NEIGHBORHOOD, (2012, unknown): “…(1995); Larsen (1996); Robin et al. (1996); Spagna et al. (1996); Ng et al. (1997); Buser et al. (1999); Ojha et al. (1999); Chiba & Beers (2000); Chen et al. (2001); López-Corredoira et al. (2002); Siegel et al. (2002); Larsen & Humphreys (2003); Cabrera-Lavers et al. (2005); Girard et al.…”
The Milky Way stellar halo out to 40 kpc: squashed, broken but smooth (2011, background): “The results are only in very rough agreemnt, suggesting that the density profile of the Milky Way has a powerlaw slope in the range2 < α < 4 and a flattening varying from 0.4 < q < 0.8 (e.g. Yanny et al. 2000; Chen et al. 2001; Newberg & Yanny 2006; Jurić et al. 2008; Sesar et al. 2011).”
Sloan Digital Sky Survey: Early Data Release (2002, background): “…galaxies (Blanton et al. 2001; Shimasaku et al. 2001; Strateva et al. 2001); the structure of the Milky Way (Ivezić et al. 2000; Yanny et al. 2000; Chen et al. 2001); the discovery of brown dwarfs (Leggett et al. 2000 and references therein); the structure of the asteroid belt (Ivezić et al.…”
THE STELLAR POPULATION STRUCTURE OF THE GALACTIC DISK (2015, methodology): “Throughout this paper, we assume that the Sun’s displacement from the mid-plane is 25 pc toward the North Galactic Pole (Chen et al. 2001; Jurić et al. 2008), and that the Sun is located at 8 kpc from the Galactic center.”
The Accretion Origin of the Milky Way’s Stellar Halo (2007, background): “This determination of halo oblateness is in excellent agreement with that of previous work (e.g., Chiba & Beers 2000; Chen et al. 2001; Larsen & Humphreys 2003; Lemon et al. 2004; Newberg & Yanny 2005; Juríc et al. 2007; Xu et al. 2006).”
RINGS AND RADIAL WAVES IN THE DISK OF THE MILKY WAY (2015, methodology): “The parameters for the thin and thick disk were chosen from the ranges presented by Chen et al. (2001).”
Empirical color transformations between SDSS photometry and Other photometric systems. (2005, background): “Transformation relations between SDSS andRGU photometry help to evaluate the earlier findings with respect to modern explorations of the structure of the Milky Way (e.g., Chen et al. (2001); Juric et al. (2005)).”
THE GENESIS OF THE MILKY WAY'S THICK DISK VIA STELLAR MIGRATION (2010, background): “…the thin disk scale height is shorter than thick disk scale height (for reviews see Majewski 1993; Buser et al. 1999; Norris 1999, and references therein), and the thick disk may have a longer scale length than the thin disk (Robin et al. 1996; Ojha 2001; Chen et al. 2001; Larsen & Humphreys 2003).”
A Matched-Filter Analysis of the Tidal Tails of the Globular Cluster Palomar 5 (2002, background): “The density ridgeline at about (g* r*) = 0.4 and about 18 < r* < 16 is probably the local thick disk population (Chen et al. 2001).”
Elemental abundance trends in the Galactic thin and thick disks as traced by nearby F and G dwarf stars (2003, background): “The normalization of the densities of the stellar populations in the solar neighbourhood gives a thick disk fraction of 2–15%, with the lowest values from Gilmore & Reid (1983) and Chen (1997), and the highest from Chen et al. (2001) and Soubiran et al. (2003).”
The stellar halo of the Galaxy (2008, methodology): “In agreement with previous work using the same technique (see previous section), Chen et al. (2001) measured n = −2.3/2.5 and q = 0.6/0.5 depending on the local normalization of the halo.”
The N2K Consortium. IV. New Temperatures and Metallicities for More than 100,000 FGK Dwarfs (2005, methodology): “Galactic structure analyses utilizing position-dependent star counts (see, e.g., Bahcall & Soneira 1981, 1984; Reid&Majewski 1993; Infante 1986, 1994; Chen et al. 1999, 2001) can be built upon immediately with the current data set and fitting framework.”
A Low-Latitude Halo Stream around the Milky Way (2003, methodology): “For the (exponential) thick disk, we use a scale height of 1.0 kpc, a scale length of 3 kpc, and a normalization of one in 30 of the thin disk star counts in the solar neighborhood (but see Chen et al. 2001).”
alpha-, r-, and s-process element trends in the Galactic thin and thick disks (2004, background): “Intermediate values∼6 % were found by Robin et al. (1996) and Buser et al. (1999), and higher values∼15 % by Chen et al. (2001) and Soubiran et al. (2003).”
Optical and Radio Properties of Extragalactic Sources Observed by the FIRST Survey and the Sloan Digital Sky Survey (2002, background): “This, plus the steeply increasing luminosity function for the less luminous red stars, gives rise to the observed bimodal stellar distribution (for details see Chen et al. 2001).”
The Emergence of the Thick Disk in a Cold Dark Matter Universe (2004, background): “The local number density of thick disk stars is about 6-13% of that of the thin disk (e.g. Chen et al. 2001); the thick disk has a scale height of 0.6-1 kpc (e.g. Phelps et al. 1999, Ojha 2001, Chen et al. 2001), about three times larger than the thin disk; a scale length of ∼ 3 kpc (e.g. Robin et…”
THE SPATIAL STRUCTURE OF MONO-ABUNDANCE SUB-POPULATIONS OF THE MILKY WAY DISK (2011, methodology): “…found that thickerdisk components have larger scale heights and longer scale lengths than their corresponding thin disk (Robin et al. 1996; Buser et al. 1999; Chen et al. 2001; Ojha 2001; Neeser et al. 2002; Larsen & Humphreys 2003; Yoachim & Dalcanton 2006; Pohlen et al. 2007; Jurić et al. 2008).”
The galaxy luminosity function at z ≃ 6 and evidence for rapid evolution in the bright end from z ≃ 7 to 5 (2014, methodology): “We adopt the main parameters of the galactic thin disk model from Chen et al. (2001), with Z = 27 ± 4pc, R = 8600 ± 200pc and hR = 2250 ± 1000 pc.”
Dissecting simulated disc galaxies - I. The structure of mono-age populations (2014, background): “The Milky Way’s thick disc not only has a larger scale-height than the thin disc (Robin et al. 1996; Chen et al. 2001; Jurić et al. 2008), but it is also older, more metal-poor, and enhanced in alpha elements (Gilmore, Wyse, & Jones 1995; Fuhrmann 1998; Prochaska et al. 2000; Bensby et al. 2005;…”