Old stellar Galactic disc in near-plane regions according to 2MASS: Scales, cut-off, flare and warp

By M. López-Corredoira, A. Cabrera-Lavers, F. Garzón, P. Hammersley. 2002

229 citations recorded by the source corpus.

We have pursued two dierent methods to analyze the old stellar population near the Galactic plane, using data from the 2MASS survey. The first method is based on the isolation of the red clump giant population in the color-magnitude diagrams and the inversion of its star counts to obtain directly the density distribution along the line of sight. The second method fits the parameters of a disc model to the star counts in 820 regions. Results from both independent methods are consistent with each other. The qualitative conclusions are that the disc is well fitted by an exponential distribution in both the galactocentric distance and height. There is not an abrupt cut-o in the stellar disc (at least within R 6 kpc) that: the scale- height in the solar circle is hz(R)= 3:6 10 2 R, the scale-length of the surface density is hR= 0:42 R and the scale-length of the space density in the plane (i.e. including the eect of the flare) is H= 0:25 R. The variation of the scale-height due to the flare follows roughly a law hz(R) hz(R )e xp R R (12 0:6R(kpc)) kpc (for R< 15 kpc; R= 7:9 kpc). The warp moves the mean position of the disc to a height zw= 1:2 10 3 R(kpc) 5:25 sin(+ 5) pc (for R< 13 kpc; R= 7:9 kpc).

Subfields: Astronomy and Astrophysics, Education

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Citations in the corpus

Outer structure of the Galactic warp and flare: explaining the Canis Major over-density (2006, methodology): “…latitude of the adopted tracer as a function of longitude (Djorgovski & Sosin 1989); (2) the ratio of star counts in Northern and Southern hemispheres as a function of longitude (López-Corredoira et al. 2002); and (3) the latitude of peak brightness as a function of longitude (Freudenreich etal.”
Dynamical Blueprints for Galaxies (2008, methodology): “Zheng et al. (2001) found Rd ¼ 2:75 0:3 kpc from HST observations of M dwarfs while López-Corredoira et al. (2002) found Rd ¼ 3:3þ0:5 0:4 kpc from an analysis of old stellar populations using 2MASS survey data.”
The UKIDSS galactic plane survey (2007, background): “They are therefore a useful tracer of stellar distance, extinction and population density, (see Lopez-Corredoira et al.2002) c© 0000 RAS, MNRAS 000, 000–000 but only in fields in which they can be distinguished from dwarfs and other types of giant.”
Infrared Extinction toward Nearby Star-forming Regions (2007, background): “We remove foreground giants by excluding any star brighter than a K2III giant with M J = −0.9 (López-Corredoira et al. 2002) at the distance of each cluster.”
Mapping the Milky Way with LAMOST– III. Complicated spatial structure in the outer disc (2018, methodology): “…complicated such that it is not a simplistic exponential nor a sech2 shape, but distorted by flaring, meaning that the scale height increases with R. López-Corredoira et al. (2002) suggested a new disc model taking into account an exponentially increasing flare along the Galactocentric radius.”
Thin, thick and dark discs in ΛCDM (2008, methodology): “11 we show the mean height of the disc along x′ – the direction of maximal height variation; the dashed line shows a fit to data from López-Corredoira et al. (2002) for the Milky Way warp: 〈z〉 = 1.2 × 10−6R(kpc)5.25 sin(φ + 5◦)kpc. (5) We average over |y′ | < 0.5 kpc and all z.”
The Milky Way’s stellar disk (2013, background): “…as a highly flattened structure with an (exponential) radial scale length of 2.5 − 3 kpc and scale height of ≃ 0.3 kpc (e.g., Kent et al. 1991; López-Corredoira et al. 2002; McMillan 2011), which is kinematically cold in the sense that the characteristic stellar velocity dispersions near…”
THE DISTANCE, MASS, AND RADIUS OF THE NEUTRON STAR IN 4U 1608−52 (2008, methodology): “The only restriction that has to be taken into account when applying this method is the contamination in the red clump counts due to dwarf stars, which is important at mK > 13 for inplane fields (López-Corredoira et al. 2002).”
The UKIRT Infrared Deep Sky Survey (UKIDSS) (2006, methodology): “Other statistical methods to measure extinction using the JHK colours alone can also be employed - see Lopez-Corredoira et al. (2002).”
The Wavelength Dependence of Interstellar Extinction from 1.25 to 8.0 μm Using GLIMPSE Data (2004, methodology): “These stars are bright enough (MJ P 1:5, e.g., López-Corredoira et al. 2002) that 2MASS and GLIMPSE can observe them to great distances through the Galactic plane.”
Mass models of the Milky Way (2011, background): “On the other hand it lies close to the scale length found by Kent, Dame, & Fazio (1991), 3 ± 0.5 kpc, and towards the lower end of the range found by López-Corredoira et al. (2002) 3.3+0.5−0.4 kpc.”
KINEMATICAL AND CHEMICAL VERTICAL STRUCTURE OF THE GALACTIC THICK DISK. II. A LACK OF DARK MATTER IN THE SOLAR NEIGHBORHOOD, (2012, unknown): “…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. (2006); Vallenari et…”
The Distribution of the Elements in the Galactic Disk (2006, background): “The stellar scale length is somewhere around 3 kpc for the Milky Way (Zheng et al. 2001; López-Corredoira et al. 2002), which implies a stellar disk of about 12 kpc based on external spirals (de Grijs et al. 2001).”
The Apache Point Observatory Galactic Evolution Experiment (APOGEE) (2007, unknown): “…al. 2004; Belokurov et al. 2006; Grillmair 2009), satellite galaxies (e.g., Willman et al. 2005; Belokurov et al. 2007), the warp of the disk (e.g., López-Corredoira et al. 2002; Reylé et al. 2009), and the still unresolved, composite anatomy of the bulge (e.g., Robin et al. 2012), which…”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, background): “…of the Southern Sky (DENIS; Ruphy et al. 1996) in the anticenter direction, COBE/FIRAS (Far Infrared Absolute Spectrophotometer; Freudenreich 1998, Drimmel & Spergel 2001), 2MASS (López-Corredoira et al. 2002, Cabrera-Lavers et al. 2005, Reylé et al. 2009), and GLIMPSE (Benjamin et al. 2005).”
Red Clump Stars from LAMOST II: the outer disc of the Milky Way (2017, methodology): “López-Corredoira et al. (2002) selected RC stars from infrared photometry, while we select them from spectroscopic data.”