TY - JOUR

T1 - Milky way kinematics. II. A uniform inner galaxy H i terminal velocity curve

AU - McClure-Griffiths, N. M.

AU - Dickey, John M.

N1 - Publisher Copyright:
© 2016. The American Astronomical Society. All rights reserved.

PY - 2016/11/10

Y1 - 2016/11/10

N2 - Using atomic hydrogen (H i) data from the VLA Galactic Plane Survey, we measure the H i terminal velocity as a function of longitude for the first quadrant of the Milky Way. We use these data, together with our previous work on the fourth Galactic quadrant, to produce a densely sampled, uniformly measured, rotation curve of the northern and southern Milky Way between 3 kpc < R < 8 kpc. We determine a new joint rotation curve fit for the first and fourth quadrants, which is consistent with the fit we published in McClure-Griffiths & Dickey and can be used for estimating kinematic distances interior to the solar circle. Structure in the rotation curves is now exquisitely well defined, showing significant velocity structure on lengths of ∼200 pc, which is much greater than the spatial resolution of the rotation curve. Furthermore, the shape of the rotation curves for the first and fourth quadrants, even after subtraction of a circular rotation fit shows a surprising degree of correlation with a roughly sinusoidal pattern between 4.2 < R < 7 kpc.

AB - Using atomic hydrogen (H i) data from the VLA Galactic Plane Survey, we measure the H i terminal velocity as a function of longitude for the first quadrant of the Milky Way. We use these data, together with our previous work on the fourth Galactic quadrant, to produce a densely sampled, uniformly measured, rotation curve of the northern and southern Milky Way between 3 kpc < R < 8 kpc. We determine a new joint rotation curve fit for the first and fourth quadrants, which is consistent with the fit we published in McClure-Griffiths & Dickey and can be used for estimating kinematic distances interior to the solar circle. Structure in the rotation curves is now exquisitely well defined, showing significant velocity structure on lengths of ∼200 pc, which is much greater than the spatial resolution of the rotation curve. Furthermore, the shape of the rotation curves for the first and fourth quadrants, even after subtraction of a circular rotation fit shows a surprising degree of correlation with a roughly sinusoidal pattern between 4.2 < R < 7 kpc.

KW - Galaxy: kinematics and dynamics

KW - ISM: kinematics and dynamics

KW - radio lines: ISM

UR - http://www.scopus.com/inward/record.url?scp=84994513751&partnerID=8YFLogxK

U2 - 10.3847/0004-637X/831/2/124

DO - 10.3847/0004-637X/831/2/124

M3 - Article

SN - 0004-637X

VL - 831

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 124

ER -