The local surface density of disc matter mapped by Hipparcos

By J. Holmberg, Chris Flynn. 2004

195 citations recorded by the source corpus.

We determine the surface density of matter in the disc of the Galaxy at the solar position using K giant stars. The local space density and luminosity function of the giants is determined using parallaxes from the Hipparcos satellite; for more distant giants, observed in a cone at the South Galactic Pole, distances are determined using intermediate-band DDO photometry (which has been calibrated to the Hipparcos absolute magnitudes). From this sample, we determine the gravitational potential vertically of the local Galactic disc, by comparing the number of giant stars observed in the cone with the number expected for various models of the matter distribution in the disc. We derive an estimate of the dynamical disc mass surface density of 56 ± 6 M ○. pc -2 , which may be compared to an estimate of 53 M ○. pc -2 in visible matter. For all gravitating matter (disc + dark halo) we find the total density within 1.1 kpc of the disc midplane to be 74 ± 6 M ○. pc -2 . As has been found by a number of studies, including our own, we find no compelling evidence for significant amounts of dark matter in the disc.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/02ec736678956e1affe426aaa2b75d7e943acd1a

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In Astronomy and Astrophysics

Citations in the corpus

Dark matter in the Milky Way II. The HI gas distribution as a tracer of the gravitational potential (2007, background): “The gravitational accelerationkz in the solar vicinity is well known from stellar statistics up to distances ofz <∼ 1.5 kpc (Kuijken & Gilmore, 1991; Holmberg & Flynn, 2000; Korchagin et al., 2003; Holmberg & Flynn, 2004), but little is known at larger distances.”
Milky Way mass models for orbit calculations (2012, background): “1 = 74 ± 6 M pc−2 from observations of K giant stars (Holmberg & Flynn 2004).”
The local dark matter density (2014, methodology): “Flynn & Fuchs (1994), Holmberg & Flynn (2000b) and Holmberg & Flynn (2004) employ a very similar method, but rather than calculating a likelihood from f(Ez), they use the 1D distribution function to calculate the density fall-off of a tracer population moving in a potential Φ(z).”
Determination of the Local Dark Matter Density in our Galaxy (2009, methodology): “eed of the solar system; 3. the total matter density at the position of the Sun from the gravitational potential determined from the movements of local stars as measured with the Hipparcos satellite (Holmberg and Flynn 2004); 4. the surface density of the visible matter at the position of the Sun (N”
ON THE LOCAL DARK MATTER DENSITY (2012, background): “…for “visual” in Figure 2) is composed of a thin 13 M⊙ pc −2 layer of interstellar medium, plus a stellar halo and “thick” and “thin” disk components with parameters taken from Jurić et al. (2008); in this model the normalization is chosen so that Σdisk(1.1 kpc) = 40M⊙ pc−2 (Holmberg & Flynn 2004).”
Constraining the thick disc formation scenario of the Milky Way (2014, unknown): “Today intermediate values given by Holmberg & Flynn (2004) of 0.102 M pc−3 and by Korchagin et al. (2003) of 0.100 M pc−3 are considered as the reference value.”
The colours of the sun (2005, background): “…(Holmberg, Portinari and Flynn, in preparation) we are determining the surface brightness of the local Galactic disc in bands from the ultraviolet (UV) to the nearinfrared (near-IR), motivated by having a good description of the mass density of its stellar content (Holmberg & Flynn 2000, 2004).”
Timing analysis for 20 millisecond pulsars in the Parkes Pulsar Timing Array (2015, background): “V08 used the Holmberg & Flynn (2004) and calculate the total galactic contribution to be Ṗ Galb = (−1.8 − 0.5) × 10−14 = −2.3 × 10−14.”
Galactic Searches for Dark Matter (2012, methodology): “Holmberg and Flynn (2004) utilized a sample of K giants selected from the Hipparcos survey.”
A new determination of the local dark matter density from the kinematics of K dwarfs (2012, methodology): “A similar result was found in the postHipparcos era by Holmberg & Flynn (2004).”
Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions (2011, background): “1 kpc) 78M⊙/pc 2 74± 6M⊙/pc(2) [194] Velocity ellipsoid tilt at z = 1 kpc 6 degrees 7.”
A General Theory of Turbulence-regulated Star Formation, from Spirals to Ultraluminous Infrared Galaxies (2005, background): “In the solar neighborhood, the total disk surface density is tot 56M pc 2 (Holmberg & Flynn 2004), and the gas surface density is g 12M pc 2 (Boulares & Cox 1990), so fg 0:21.”
STARS, GAS, AND DARK MATTER IN THE SOLAR NEIGHBORHOOD (2015, methodology): “Holmberg & Flynn (2004) introduced a thick stellar disk in their model for the vertical distribution of stars.”
Precision Timing of PSR J0437–4715: An Accurate Pulsar Distance, a High Pulsar Mass, and a Limit on the Variation of Newton’s Gravitational Constant (2008, methodology): “Acceleration in the Galactic gravitational potential varies as a function of height above the Galactic plane (Holmberg & Flynn 2004), which may be estimated using the parallax distance and the Galactic latitude of the pulsar.”
The Milky Way’s stellar disk (2013, methodology): “A number of conceptually similar analyses have been carried out since (e.g., Flynn & Fuchs 1994; Siebert et al. 2003; Holmberg & Flynn 2004): these confirmed the approximate values for Σ<1 kpc, and Siebert et al. (2003) obtained a first constraint on the dynamical thickness of the stellar disk…”
On the mass-to-light ratio of the local Galactic disc and the optical luminosity of the Galaxy (2006, methodology): “It is also compatible, though on the lower end of the uncertainty range, with the more recent, Hipparcos-based dynamical estimate of the surface density 56 ± 6 M pc−2 (Holmberg & Flynn 2000, 2004).”
REGULATION OF STAR FORMATION RATES IN MULTIPHASE GALACTIC DISKS: A THERMAL/DYNAMICAL EQUILIBRIUM MODEL (2010, background): “For the local Milky Way, which has ρs = 0.04 M⊙ pc −3 (Holmberg & Flynn 2000) and Σs = 42 M⊙ pc −2 (Holmberg & Flynn 2004) from dynamical mass models, a scale length of Rs = 2.6 kpc (Jurić et al. 2008) would yield Σs/(0.54Rs) = 0.03 M⊙ pc −3.”