Galactic Interior Motions Derived from [ITAL]Hipparcos[/ITAL] Proper Motions. I. Young Disk Population

Miyamoto, M.; Zhu, Zi

doi:10.1086/300292

Cited by 75 publications

(51 citation statements)

References 8 publications

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“…It is a high value but in agreement with recent studies of OYB5 star samples from the Hipparcos catalog by Miyamoto & Zhu (1998), Â ¼268:7AE11:9 km s À1 ; Uemura et al (2000), Â ¼ 255:52 AE 8:33 km s À1 ; or Branham (2002), Â ¼ 258:7 AE 34:29 km s À1 . A similar result (Â ¼ 270 km s À1 ) is also reached by Méndez et al (2000) using data from the Southern Proper Motion Catalog ( Platais et al 1998); thus, their result is obtained from measures of the proper motions independent of those from Hipparcos.…”

Section: Estimation Of the Oort Constantssupporting

confidence: 91%

OB Stars in the Solar Neighborhood. II. Kinematics

2006

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Using the spatial classification method and the structural parameters estimated for the Gould Belt (GB) and the local Galactic disk ( LGD) from a previous paper, we have evaluated spatial membership probabilities for a sample of O and B stars from the Hipparcos catalog ( Perryman and coworkers) with available proper motions and radial velocity data. Thus, being able to study the space velocity fields of both systems, we conclude that the GB and the LGD present different statistical distributions, both in velocity space and in phase space. In light of their possible existence as distinct systems, we analyze different kinematic aspects in the vicinity of the Sun, and we find the GB to be responsible for the highly negative vertex deviation found for the OB stars in the solar neighborhood. We also find that the GB noticeably alters the estimation of the Oort constants in the Galactic disk; thus, in order to establish comparisons with other kinematic studies based on older stellar populations, a careful pruning of the GB members must be performed. Further analysis of the GB velocity field and the moving groups that contribute to it suggest the possibility that the GB can be the result of a chance superposition of moving groups. We propose for future investigations the dynamical analysis of these moving groups in order to probe the origin of the GB.

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Section: Estimation Of the Oort Constantssupporting

confidence: 91%

OB Stars in the Solar Neighborhood. II. Kinematics

2006

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“…), T < 4.64 Gyr (95.4% C.L.). Our results are equivalent to a rotation of the rings around the line of nodes with an angular velocity oḟ result of +4 km s −1 /kpc given by Miyamoto et al (1993) or Miyamoto & Zhu (1998) at short distances from the Sun, but it is more similar to the result of −4 km s −1 /kpc by Bobylev (2010), who also used RGCs. Bobylev (2013) obtained with Cepheids a value of −15 km s −1 /kpc, which is different from our result.…”

Section: We Can Derive Some Information Of the Warp Kinematicssupporting

confidence: 72%

Vertical velocities from proper motions of red clump giants

López-Corredoira

Abedi

Garzón

et al. 2014

A&A

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Aims. We derive the vertical velocities of disk stars in the range of Galactocentric radii of R = 5−16 kpc within 2 kpc in height from the Galactic plane. This kinematic information is connected to dynamical aspects in the formation and evolution of the Milky Way, such as the passage of satellites and vertical resonance and determines whether the warp is a long-lived or a transient feature. Methods. We used the PPMXL survey, which contains the USNO-B1 proper motions catalog cross-correlated with the astrometry and near-infrared photometry of the 2MASS point source catalog. To improve the accuracy of the proper motions, the systematic shifts from zero were calculated by using the average proper motions of quasars in this PPMXL survey, and we applied the corresponding correction to the proper motions of the whole survey, which reduces the systematic error. From the color-magnitude diagram K versus (J − K) we selected the standard candles corresponding to red clump giants and used the information of their proper motions to build a map of the vertical motions of our Galaxy. We derived the kinematics of the warp both analytically and through a particle simulation to fit these data. Complementarily, we also carried out the same analysis with red clump giants spectroscopically selected with APOGEE data, and we predict the improvements in accuracy that will be reached with future Gaia data. Results. A simple model of warp with the height of the disk z w (R, φ) = γ(R − R ) sin(φ − φ w ) fits the vertical motions ifγ/γ = −34 ± 17 Gyr −1 ; the contribution toγ comes from the southern warp and is negligible in the north. If we assume this 2σ detection to be real, the period of this oscillation is shorter than 0.43 Gyr at 68.3% C.L. and shorter than 4.64 Gyr at 95.4% C.L., which excludes with high confidence the slow variations (periods longer than 5 Gyr) that correspond to long-lived features. Our particle simulation also indicates a probable abrupt decrease of the warp amplitude in a time of about one hundred Myr. Conclusions. The vertical motion in the warp apparently indicates that the main S-shaped structure of the warp is a long-lived feature, whereas the perturbation that produces an irregularity in the southern part is most likely a transient phenomenon. But we need higher accuracy in the systematic errors of proper motions to confirm this tentative detection of vertical motion in the outer disk. With the use of the Gaia end-of-mission products together with spectroscopically classified red clump giants, the precision in vertical motions can be increased by an order of magnitude at least.

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“…If we take Kerr & Lynden-Bell's (1986) distance to the Galactic center of 8:5 AE 1:1 kpc, the values for the Oort constants imply a circular motion near the values found by Miyamoto & Zi (1998) and Zhu & Jin (2000), but with higher mean error, and higher than the IAU's recommended 220 AE 20 km s À1 . This discrepancy, however, is more apparent than real.…”

Section: Discussionsupporting

confidence: 56%

“…When analyzing Hipparcos proper motions for 1352 nonGould Belt O-B5 stars, Miyamoto & Zi (1998) find a large Galactic rotation of 268:7 AE 11:9 km s À1 , higher than the IAU's recommended 220 AE 20 km s À1 . Zhu & Jin (2000), likewise using Hipparcos proper motions but also adding radial velocities, find virtually the same Galactic rotation.…”

Section: Introductionmentioning

confidence: 78%

Kinematics of OB Stars

Branham¹

2002

ApJ

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The kinematics of 1817 stars of class O-B5 are examined. The 1655 stars with distances up to 1 kpc are taken from the Hipparcos catalog and 162 stars with distances greater than 1 kpc from Westlin's study of OB stars. The Ogorodnikov-Milne model of Galactic kinematics, with Edmondson's second-order terms included, is used for the equations of condition and mixed total least squares-least squares (TLS-LS) is used for the reduction method. Reasonable values for the parameters of Galactic kinematics are obtained. In particular, Oort A and B constants yield a Galactic rotation of 258:7 AE 34:29 km s À1 if we take the distance of the Sun from the Galactic center as 8:5 AE 1:1 kpc. Although lower than the higher values obtained by some other investigators and higher than the IAU's recommended 220 AE 20 km s À1 , all the determinations fall with their stated mean errors. Thus, no evidence for a significant difference in the various determinations exists. Evidence does exist, however, to assert that the TLS-LS reduction model with second-order terms seems superior to ordinary least-squares with only first-order terms.

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Galactic Interior Motions Derived from [ITAL]Hipparcos[/ITAL] Proper Motions. I. Young Disk Population

Cited by 75 publications

References 8 publications

OB Stars in the Solar Neighborhood. II. Kinematics

OB Stars in the Solar Neighborhood. II. Kinematics

Vertical velocities from proper motions of red clump giants

Kinematics of OB Stars

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