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J/ApJ/785/63        Rotation curve of the Milky Way       (Bhattacharjee+, 2014)

Rotation curve of the Milky Way out to ∼200 kpc. Bhattacharjee P., Chaudhury S., Kundu S. <Astrophys. J., 785, 63 (2014)> =2014ApJ...785...63B (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Galaxies, rotation ; Sun ; Stars, distances ; Rotational velocities Keywords: dark matter - Galaxy: general - Galaxy: kinematics and dynamics Abstract: The rotation curve (RC) of our Galaxy, the Milky Way, is constructed starting from its very inner regions (few hundred parsecs) out to a large galactocentric distance of ∼200 kpc using kinematical data on a variety of tracer objects moving in the gravitational potential of the Galaxy, without assuming any theoretical models of the visible and dark matter (DM) components of the Galaxy. We study the effect on the RC due to the uncertainties in the values of the Galactic constants (GCs) R0 and V0 (these being the Sun's distance from and circular rotation speed around the Galactic center, respectively) and the velocity anisotropy parameter β of the halo tracer objects used for deriving the RC at large galactocentric distances. The resulting RC in the disk region is found to depend significantly on the choice of the GCs, while the dominant uncertainty in the RC at large distances beyond the stellar disk comes from the uncertainty in the value of β. In general we find that the mean RC steadily declines at distances beyond ∼60 kpc, independently of the value of β. Also, at a given radius, the circular speed is lower for larger values of β (i.e., for more radially biased velocity anisotropy). Considering that the largest possible value of β is unity, which corresponds to stellar orbits being purely radial, our results for the case of β=1 give a lower limit to the total mass of the Galaxy within ∼200 kpc, M(200 kpc)≳(6.8±4.1)x1011 M, independently of any model of the DM halo of the Galaxy. Description: In this paper, we consider a combination of currently available large samples of a variety of both disk and non-disk tracers to construct the rotation curve (RC) of the Galaxy from ∼0.2 kpc to ∼200 kpc. We perform a detailed analysis of the dependence of the RC on the choice of the Galactic constants (GCs) and also the dependence on the anisotropy parameter β of the non-disk tracers. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 28 151 Rotation Curve of the Milky Way
See also: VII/70 : Galaxies Rotation Curves (Baiesi-Pillastrini+ 1983) J/A+A/275/67 : Velocity Field of the outer Galaxy (Brand+ 1993) J/AJ/139/59 : Milky Way halo velocity dispersion profile (Brown+, 2010) J/ApJ/714/1170 : Faraday rotation at high Galactic latitude (Mao+, 2010) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 F3.1 kpc R0 Sun's distance from Galactic center 5- 7 I3 km/s V0 Sun's circular rotation velocity around Galactic center 9- 14 F6.2 kpc r Distance from Galactic center 16- 21 F6.2 km/s Vc Circular velocity 23- 28 F6.2 km/s e_Vc The 1-σ error in Vc
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 28-Jun-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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