Global properties of the H I distribution in the outer Milky Way - Planar and extra-planar gas

By P. Kalberla, L. Dedes. 2008

168 citations recorded by the source corpus.

Context. The determination of the global structure of the planar and extra-planar Milky Way H i disk depends critically on a reliable database but also on reasonable assumptions about the shape of the Milky Way rotation curve. Aims. We derive the 3D H i volume density distribution for the Galactic disk out to R ∼ 60 kpc. Methods. Our analysis is based on parameters for the warp and rotation curve derived previously. The data are taken from the Leiden/Argentine/Bonn all sky 21 cm line survey. Results. The Milky Way H i disk is significantly warped but shows a coherent structure out to R ∼ 35 kpc. The radial surface density distribution, the densities in the middle of the warped plane, and the H i scale heights all follow exponential relations. The radial scale length for the surface density distribution of the H i disk is 3.75 kpc. Gas at the outskirts for 40 15 kpc there is more gas in the south. The H i flaring indicates that this asymmetry is caused by a dark matter wake, located at R ∼ 25 kpc in direction of the Magellanic System. Conclusions. The H i disk is made up of two major components. Most prominent is the normal H i disk which can be traced to R ∼ 35 kpc. This is surrounded by a patchy distribution of highly turbulent gas reaching large scale heights but also large radial distances. At the position of the Sun the exponential scale height in the z direction is 3.9 kpc. This component resembles the anomalous gas discovered previously in some galaxies.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/6beca1487a32bb9463d3390f505daefc8228fc0e

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Citations in the corpus

The SILCC project - III. Regulation of star formation and outflows by stellar winds and supernovae (2016, background): “…particular, SN explosions can create a hot ionized medium (Cox & Smith 1974; McKee & Ostriker 1977) with high volume-filling factors (Ferrière 2001; Kalberla & Dedes 2008; Walch et al. 2015), which may launch powerful outflows from galactic discs (e.g. Oppenheimer et al. 2010; Creasey, Theuns &…”
Painting a portrait of the Galactic disc with its stellar clusters (2020, unknown): “Our simple model assumes a linear increase in the scale height with Galactocentric radius, A1, page 12 of 17 but Kalberla et al. (2007) and Kalberla & Dedes (2008), who could trace atomic hydrogen out to much larger distances than our cluster sample, show that the flaring of HI gas outside the…”
Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation (2013, methodology): “Aiming to separate Galactic emission from the observations of the Magellanic system we calculated the expected Milky Way emission according to the model of Kalberla & Dedes (2008).”
The H i Distribution of the Milky Way (2009, methodology): “A Average flaring of the Hi gas layer as a function of R (from Kalberla & Dedes 2008).”
DOES THE STELLAR DISTRIBUTION FLARE? A COMPARISON OF STELLAR SCALE HEIGHTS WITH LAB H i DATA (2014, methodology): “At larger distances the H i data show a considerable scatter with systematic deviations between the northern and southern hemispheres, while the model is axisymmetric (Kalberla & Dedes 2008, Figure 4).”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, background): “Major reviews of the stellar disk include those by Freeman & Bland-Hawthorn (2002), Ivezić et al. (2012), and Rix & Bovy (2013); the gaseous disk is discussed at length by Kalberla & Dedes (2008).”
The local dark matter density (2014, methodology): “Holmberg & Flynn (2000a) split the HI into hot and cold components that each contribute ΣHI ∼ 4 M pc−2 (see Table 2), whereas Wolfire et al. (2003) favour ΣHI ∼ 5 M pc−2, and Kalberla & Dedes (2008) ΣHI ∼ 12 M pc−2.”
The Nine Lives of Cosmic Rays in Galaxies (2015, background): “By the end of their journey, they have traversed a gas column density NH ≈ 3× 1024 cm−2, which largely exceeds the disc-through integrals of (0.1– 1.4)× 1021 cm−2 characterizing the ISM to a radius of 20 kpc (Kalberla & Dedes 2008, Pineda et al. 2013).”
The milky way total mass profile as inferred from Gaia DR2 (2019, methodology): “The next two components of the MW are the HI and the molecular gas distributions, which can account for a significant fraction of the baryonic mass and, since they have a different geometry from the stellar component, cannot be easily treated as part of the stellar disc (Kalberla & Dedes 2008).”
Chemical evolution with radial mixing (2008, background): “Our value for the scalelength of the gas disc is in good agreement with the value measured by Kalberla & Dedes (2008): 3.75 kpc. Note that we assume not only that the stellar disc is exponential, but also that its scalelength is unchanging.”
STARS, GAS, AND DARK MATTER IN THE SOLAR NEIGHBORHOOD (2015, methodology): “This is essentially the same as the value of M8 pc 2- given by Kulkarni & Heiles (1987) and is quite close to the value of M9 pc 2- cited by Kalberla (private communication) based on the data in Kalberla & Dedes (2008).”
Molecular Clouds in the Milky Way (2015, background): “More recent estimates of the inner Galaxy H2 mass are much lower (∼ 0.7 × 109 M ; see Section 4.6), and a recent analysis of the Leiden/Argentine/Bonn HI survey suggests that the inner Galaxy HI mass may be significantly higher than has normally been assumed, ∼1.8×109 M (Kalberla & Dedes 2008).”
THE COS-HALOS SURVEY: RATIONALE, DESIGN, AND A CENSUS OF CIRCUMGALACTIC NEUTRAL HYDROGEN (2013, methodology): “Kalberla & Dedes (2008) treat this as an extension of the main disk, but one which may consist of numerous small clouds or a turbulent medium with high velocity dispersion.”
Gaseous Galaxy Halos (2012, background): “In some regions, there are kpc extensions from the disk due to the presence of IVCs or the Galactic warp (Levine et al., 2006; Kalberla & Dedes, 2008).”
Star Formation in the Milky Way and Nearby Galaxies (2012, methodology): “Based on a model including dark matter (Kalberla & Kerp 2009; Kalberla et al. 2007; Kalberla & Dedes 2008), the MW mass within 60 kpc of the center is M(tot) = 4.6× 1011 M⊙, with M(baryon) = 9.5× 10 10 M⊙.”