Galactic masers: Kinematics, spiral structure and the disk dynamic state

Rastorguev, A. S.; Utkin, N. D.; Zabolotskikh, M. V.; Дамбис, А. К.; Bajkova, A. T.; Бобылев, В. В.

doi:10.1134/s1990341317020043

Cited by 76 publications

(62 citation statements)

References 111 publications

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“…Since the orbits of the open clusters studied here are confined within this range, the shape of the rotation curve outside this interval has no influence. As examples of recently measured curves, see the one derived from maser sources (Rastorguev et al 2017), that derived from the SEGUE and RAVE surveys (Sysoliatina et al 2018), and from GAIA DR2 (Crosta et al 2018). The new results are not discrepant with the older ones, like the HI + CO rotation curve of Fich et al (1989) and those determined from high mass star forming regions with measured parallax and proper motion by Reid et al (2014).…”

Section: The Orbits Of the Open Clusters And The Galactic Rotation Curvementioning

confidence: 99%

The spiral pattern rotation speed of the Galaxy and the corotation radius with Gaia DR2

Dias

Monteiro

Lépine

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In this work we revisit the issue of the rotation speed of the spiral arms and the location of the corotation radius of our Galaxy. This research was performed using homogeneous data set of young open clusters (age < 50 Myr) determined from Gaia DR2 data. The stellar astrometric membership were determined using proper motions and parallaxes, taking into account the full covariance matrix. The distance, age, reddening and metallicity of the clusters were determined by our non subjective multidimensional global optimization tool to fit theoretical isochrones to Gaia DR2 photometric data. The rotation speed of the arms is obtained from the relation between age and angular distance of the birthplace of the clusters to the present-day position of the arms. Using the clusters belonging to the Sagittarius-Carina, Local and Perseus arms, and adopting the Galactic parameters R 0 = 8.3 kpc and V 0 = 240 km s −1 , we determine a pattern speed of 28.2 ± 2.1 km s −1 kpc −1 , with no difference between the arms. This implies that the corotation radius is R c = 8.51 ± 0.64 kpc, close to the solar Galactic orbit (R c /R 0 = 1.02 ± 0.07).

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Section: The Orbits Of the Open Clusters And The Galactic Rotation Curvementioning

confidence: 99%

The spiral pattern rotation speed of the Galaxy and the corotation radius with Gaia DR2

Dias

Monteiro

Lépine

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Here we use the following parameter values: M disk = 10 11 M sun , a = 5, b = 0.26, M spher = 3.4 × 10 10 M sun , c = We choose these constants so as to ensure that the resulting rotation curve in the Galactic disk would fit the rotation curve based on recent data about the kinematics of Galactic masers [21], implying a circular velocity rotation of about 237 km/s at the solar circle (we adopt R 0 = 8.3 kpc throughout this paper).…”

Section: Galactic Potential Modelmentioning

confidence: 99%

Globular Clusters: Absolute Proper Motions and Galactic Orbits

et al. 2018

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We cross-match objects from several different astronomical catalogs to determine the absolute proper proper motions of stars within the 30-arcmin radius fields of 115 Milky-Way globular clusters with the accuracy of 1-2 mas/yr. The proper motions are based on positional data recovered from the USNO-B1, 2MASS, URAT1, ALLWISE, UCAC5, and GAIA DR1 surveys with up to 10 positions spanning an epoch difference of up to ∼ 65 years, and reduced to GAIA DR1 TGAS frame using UCAC5 as the reference catalog. Cluster members are photometrically identified by selecting horizontal-and red-giant branch stars on color-magnitude diagrams, and the mean absolute proper motions of the clusters with a typical formal error of ∼ 0.4 mas/yr are computed by averaging the proper motions of selected members. The inferred absolute proper motions of clusters are combined with available radial-velocity data and heliocentric distance estimates to compute the cluster orbits in terms of the Galactic potential models based on Miyamoto and Nagai disk, Hernquist spheroid, and modified isothermal dark-matter halo (axisymmetric model without a bar) and the same model + rotating Ferre's bar (non-axisymmetric). Five distant clusters have higher-than-escape velocities, most likely due to large errors of computed transversal velocities, whereas the computed orbits of all other clusters remain bound to the Galaxy. Unlike previously published results, we find the bar to affect substantially the orbits of most of the clusters, even those at large Galactocentric distances, bringing appreciable chaotization, especially in the portions of the orbits close to the Galactic center, and stretching out the orbits of some of the thick-disk clusters.

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“…Here the linear rotation speed of the Sun around the center of the Galaxy is V 0 = 210 ± 6 km/s (for adopted R 0 = 8.0 ± 0.2 kpc). It is interesting to compare the parameters for the galactic rotation obtained here with, for example, the estimates of Rastorguev, et al [36] derived from data on 136 masers with measured trigonometric parallaxes covering a wide range of distances R : 0- (for the found R 0 = 8.34 ± 0.16 kpc). Based on the velocities of 260 Cepheids with proper motions from the Gaia DR1 catalog, it was found [28] Table 2 of [22]), fairly low values of the angular rotation speed, Ω ∼ 24 km/s/kpc, were found.…”

Section: Resultsmentioning

confidence: 62%

Galactic Kinematics Derived From Data in the RAVE5, UCAC4, PPMXL, and Gaia TGAS Catalogs

et al. 2017

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The spatial velocities of the stars with high-precision positions, proper motions and parallaxes from the Gaia TGAS catalog and line-of-sight velocities from the RAVE5 catalog are considered. From the sample of 92395 stars with the age estimates we have obtained the following kinematic parameters: (U, V, W ) = (9.42, 20.34, 7.21) ± (0.12, 0.10, 0.09) km s −1 , Ω = 26.29 ± 0.39 km s −1 kpc −1 and Ω ′ = −3.89 ± 0.08 km s −1 kpc −2 , where V 0 = 210 ± 6 km s −1 (for adopted R 0 = 8.0 ± 0.2 kpc), and the Oort constants A = 15.57±0.31 km s −1 kpc −1 and B = −10.72±0.50 km s −1 kpc −1 . It is shown that the parameters Ω and Ω ′ are stable to the star age. A comparative analysis of the Bottlinger model parameters obtained separately from the RAVE5 catalog line-of-sight velocities and the Gaia TGAS, UCAC4 and PPMXL catalogs proper motion has been made. It is shown that these parameters are in good agreement with each other when derived from the proper motions of both the terrestrial catalogs and catalog Gaia TGAS. At the same time, it was established that the values of the Bottlinger model parameters obtained from the line-of-sight velocities can differ from the corresponding parameters obtained from the proper motions. The reduction of the line-of-sight velocities from the RAVE5 catalog is proposed for eliminating these differences.

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Galactic masers: Kinematics, spiral structure and the disk dynamic state

Cited by 76 publications

References 111 publications

The spiral pattern rotation speed of the Galaxy and the corotation radius with Gaia DR2

The spiral pattern rotation speed of the Galaxy and the corotation radius with Gaia DR2

Globular Clusters: Absolute Proper Motions and Galactic Orbits

Galactic Kinematics Derived From Data in the RAVE5, UCAC4, PPMXL, and Gaia TGAS Catalogs

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