We compile and analyze ~200 trigonometric parallaxes and proper motions of molecular masers associated with very young high-mass stars. These measurements strongly suggest that the Milky Way is a four-arm spiral. Fitting log-periodic spirals to the locations of the masers, allows us to significantly expand our view of the structure of the Milky Way. We present an updated model for its spiral structure and incorporate it into our previously published parallax-based distance-estimation program for sources associated with spiral arms. Modeling the three-dimensional space motions yields estimates of the distance to the Galactic center, Ro = 8.15 +/- 0.15 kpc, the circular rotation speed at the Sun's position, To = 236 +/- 7 km/s, and the nature of the rotation curve. Our data strongly constrain the full circular velocity of the Sun, To + Vsun = 247 +/- 4 km/s, and its angular velocity, (To + Vsun)/Ro = 30.32 +/- 0.27 km/s/kpc. Transforming the measured space motions to a Galactocentric frame which rotates with the Galaxy, we find non-circular velocity components typically about 10 km/s. However, near the Galactic bar and in a portion of the Perseus arm, we find significantly larger non-circular motions. Young high-mass stars within 7 kpc of the Galactic center have a scale height of only 19 pc and, thus, are well suited to define the Galactic plane. We find that the orientation of the plane is consistent with the IAU-defined plane to within +/-0.1 deg., and that the Sun is offset toward the north Galactic pole by Zsun = 5.5 +/- 5.8 pc. Accounting for this offset places the central supermassive black hole, Sgr A*, in the midplane of the Galaxy. Using our improved Galactic parameters, we predict the Hulse-Taylor binary pulsar to be at a distance of 6.54 +/- 0.24 kpc, assuming its orbital decay from gravitational radiation follows general relativity.

Trigonometric Parallaxes Of High-Mass Star Forming Regions: Our View Of The Milky Way

We compile and analyze approximately 200 trigonometric parallaxes and proper motions of molecular masers associated with very young high-mass stars. Most of the measurements come from the BeSSeL Survey using the VLBA and the Japanese VERA project. These measurements strongly suggest that the Milky Way is a four-arm spiral, with some extra arm segments and spurs. Fitting log-periodic spirals to the locations of the masers, allowing for ?kinks? in the spirals and using well-established arm tangencies in the fourth Galactic quadrant, allows us to significantly expand our view of the structure of the Milky Way. We present an updated model for its spiral structure and incorporate it into our previously published parallax-based distance-estimation program for sources associated with spiral arms. Modeling the three-dimensional space motions yields estimates of the distance to the Galactic center, <CDATA<i, the circular rotation speed at the Sun's position, <CDATA<i km;s(?1), and the nature of the rotation curve. Our data strongly constrain the full circular velocity of the Sun, <CDATA<i km;s(?1), and its angular velocity, <CDATA<i km;s(?1) kpc(?1). Transforming the measured space motions to a Galactocentric frame which rotates with the Galaxy, we find non-circular velocity components typically ?10 km;s(?1). However, near the Galactic bar and in a portion of the Perseus arm we find significantly larger non-circular motions. Young high-mass stars within 7 kpc of the Galactic center have a scale height of only 19 pc, and thus are well suited to define the Galactic plane. We find that the orientation of the plane is consistent with the IAU-defined plane to within;01, and that the Sun is offset toward the north Galactic pole by <CDATA<i pc. Accounting for this offset places the central supermassive black hole, Sgr;A*, in the midplane of the Galaxy. The measured motions perpendicular to the plane of the Galaxy limit precession of the plane to ?4 km;s(?1) at the radius of the Sun. Using our improved Galactic parameters, we predict the Hulse?Taylor binary pulsar to be at a distance of 6.54;;0.24 kpc, assuming its orbital decay from gravitational radiation follows general relativity.

https://iopscience.iop.org/article/10.3847/1538-4357/ab4a11/pdf

Trigonometric Parallaxes of High-mass Star-forming Regions : Our View of the Milky Way

We report trigonometric parallaxes for water masers in the G012.88+0.48 region and in the massive star forming complex W33 (containing G012.68−0.18, G012.81−0.19, G012.90−0.24, G012.90−0.26), from the Bar and Spiral Structure Legacy (BeSSeL) survey using the Very Long Baseline Array. The parallax distances to all these masers are consistent with kpc, which locates the W33 complex and G012.88+0.48 in the Scutum spiral arm. Our results show that W33 is a single star forming complex at about two-thirds the kinematic distance of 3.7 kpc. The luminosity and mass of this region, based on the kinematic distance, have therefore been overestimated by more than a factor of two. The spectral types in the star cluster in W33 Main have to be changed by 1.5 points to later types.

/pdf/trigonometric-parallaxes-of-massive-star-forming-regions-1fugu5yvwd.pdf

Trigonometric Parallaxes of Massive Star Forming Regions: G012.88+0.48 and W33

We applied the currently most comprehensive version of the statistical-parallax technique to derive the kinematical parameters of the maser sample with 136 sources. Our kinematic model comprises the overall rotation of the Galactic disk and the spiral density-wave effects, and the variation of radial velocity dispersion with Galactocentric distance. The best description of the observed velocity field is provided by the model with constant radial and vertical velocity dispersions, (σU0, σW0) ≈ (9.4 ± 0.9, 5.9 ± 0.8) kms−1. The resulting Galactic rotation curve proved to be flat over the Galactocentric distance interval from 3 to 15 kpc and we find the local circular rotation velocity to be V
 0 ≈ (235 − 238) ± 7 km s−1. We determine the parameters of the four-armed spiral pattern (pitch angle i ≈ −10. ◦ 4 ± 0.3◦ and the phase of the Sun χ0 ≈ 125◦ ± 10◦). The amplitudes of radial and tangential spiral perturbations are about f
 R ≈ −6.9 ± 1.4 km s−1, f
 Θ ≈ +2.8 ± 1.0 km s−1. The kinematic data yield a solar Galactocentric distance of R
 0 ≈ 8.24 ± 0.12 kpc. Based on rotation curve parameters and the asymmetric drift we infer the exponential disk scale H
 D ≈ 2.7 ± 0.2 kpc assuming marginal stability of the intermediate-age disk, and also estimate the minimum local surface disk density, Σ(R
 0) > 26 ± 3M
 ⊙ pc−2.

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

An up-to-date overview of the recent history is given, aiming is to present a helpful working guide to the literature and at the same time introduce key systems and observational results, starting ...

https://tandfonline.com/doi/pdf/10.1080/21672857.2017.1379459

A guided map to the spiral arms in the galactic disk of the Milky Way

We have conducted the first parallax and proper motion measurements of 6.7 GHz methanol maser emission using the Australian Long Baseline Array. The parallax of G 339.884-1.259 measured from five epochs of observations is 0.48 +/- 0.08 mas, corresponding to a distance of 2.1(-0.3)(+0.4) kpc, placing it in the Scutum spiral arm. This is consistent (within the combined uncertainty) with the kinematic distance estimate for this source at 2.5 +/- 0.5 kpc using the latest Solar and Galactic rotation parameters. We find from the Lyman continuum photon flux that the embedded core of the young star is of spectral type B1, demonstrating that luminous 6.7 GHz methanol masers can be associated with high-mass stars toward the lower end of the mass range.

/pdf/first-parallax-measurements-toward-a-6-7-ghz-methanol-maser-4n9amhawq2.pdf

FIRST PARALLAX MEASUREMENTS TOWARD A 6.7 GHz METHANOL MASER WITH THE AUSTRALIAN LONG BASELINE ARRAY-DISTANCE TO G 339.884-1.259

We report the first Very Long Baseline Array (VLBA) observations of v = 1, J = 1-0 SiO masers at 43 GHz in the circumstellar envelope of the M-type semiregular supergiant variable star AH Sco at two epochs separated by 12 days in 2004 March. These high-resolution VLBA images reveal that the distribution of the SiO masers is roughly on a persistent elliptical ring, with the lengths of the major and minor axes being about 18.5 and 15.8 mas, respectively, along a position angle of 150 degrees. The redshifted masers are found to be slightly closer to the central star than are the blueshifted masers. The line-of-sight velocity structure of the SiO masers shows that with respect to the systemic velocity of -6.8 km s(-1), the higher velocity features are closer to the star, which can be well explained by the simple outflow or infall, without rotation kinematics, of SiO masers around AH Sco. A study of the proper motions of 59 matched features between our two epochs clearly indicates that the SiO maser shell around AH Sco was undergoing an overall contraction toward the star at a velocity of approximate to 13 km s(-1) at a distance of 2.26 kpc to AH Sco. Our three-dimensional maser kinematics model further suggests that such an inward motion is very likely to be due to the gravitation of the central star. The distance to AH Sco of 2.26 +/- 0.19 kpc that we obtained from our three-dimensional kinematics model fitting is consistent with its kinematic distance of 2.0 kpc.

VLBI OBSERVATIONS OF SiO MASERS AROUND AH SCORPII

Abstract We present VLBI maps of the 6.7 GHz methanol maser emission in 32 sources obtained using the Japanese VLBI Network (JVN) and the East-Asian VLBI Network (EAVN). All of the observed sources provide new VLBI maps, and the spatial morphologies have been classified into five categories similar to the results obtained from European VLBI Network observations (Bartkiewicz et al. 2009). The 32 methanol sources are being monitored to measure the relative proper motions of the methanol maser spots.

/pdf/the-vlbi-mapping-survey-of-the-6-7-ghz-methanol-masers-with-20ssbzau6d.pdf

Xi Chen

Papers

FIRST PARALLAX MEASUREMENTS TOWARD A 6.7 GHz METHANOL MASER WITH THE AUSTRALIAN LONG BASELINE ARRAY-DISTANCE TO G 339.884-1.259

VLBI OBSERVATIONS OF SiO MASERS AROUND AH SCORPII

The VLBI mapping survey of the 6.7 GHz methanol masers with the JVN/EAVN