Astrometry of Galactic Star-Forming Region Sharpless 269 with VERA: Parallax Measurements and Constraint on Outer Rotation Curve

Honma, Mareki; Bushimata, Takeshi; Choi, Yoon Kyung; Hirota, Tomoya; Imai, Hiroshi; Iwadate, Kenzaburo; Jike, Takaaki; Kameya, Osamu; Kamohara, Ryuichi; Kan-ya, Yukitoshi; Kawaguchi, Noriyuki; Kijima, Minoru; Kobayashi, Hideyuki; Kuji, Seisuke; Kurayama, Tomoharu; Manabe, S.; Miyaji, Takeshi; Nagayama, Tomonori; Nakagawa, Akiharu; Oh, Chung Sik; Omodaká, Toshihiro; Oyama, Tomoaki; Sakai, Satoshi; Sato, Katsuhisa; Sasao, Tetsuo; Shibata, Katsunori M.; Shintani, Motonobu; Suda, Hiroshi; Tamura, Yoshiaki; Tsushima, Miyuki; Yamashita, K.

doi:10.1093/pasj/59.5.889

Cited by 124 publications

(40 citation statements)

References 29 publications

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“…The latest modeling indicates that R0 = 8.35 ± 0.16 kpc and Θ0 = 251 ± 8 km s −1 (Reid et al 2014). Also, the rotation curve between 4 and 13 kpc from the Galactic center is very flat (Honma et al 2007;Reid et al 2014). Such a large value for Θ0 (about 15% larger than the IAU recommended value of 220 km s −1 ), if confirmed by other measurements, would have widespread impact in astrophysics, including increasing the total mass (including dark matter halo) of the Milky Way by about 50%, revising Local Group dynamics by changing the Milky Way's mass and velocities of Group members (when transforming from Heliocentric to Galactocentric coordinate systems), and increasing the expected signal from dark matter annihilation radiation.…”

Section: Galactic Structurementioning

confidence: 99%

Microarcsecond Radio Astrometry

Reid

Honma

2014

Annu. Rev. Astron. Astrophys.

177

191

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Astrometry provides the foundation for astrophysics. Accurate positions are required for the association of sources detected at different times or wavelengths, and distances are essential to estimate the size, luminosity, mass, and ages of most objects. Very Long Baseline Interferometry at radio wavelengths, with diffraction-limited imaging at sub-milliarcsec resolution, has long held the promise of micro-arcsecond astrometry. However, only in the past decade has this been routinely achieved. Currently, parallaxes for sources across the Milky Way are being measured with ∼ 10 µas accuracy and proper motions of galaxies are being determined with accuracies of ∼ 1 µas y −1 . The astrophysical applications of these measurements cover many fields, including star formation, evolved stars, stellar and super-massive black holes, Galactic structure, the history and fate of the Local Group, the Hubble constant, and tests of general relativity. This review summarizes the methods used and the astrophysical applications of micro-arcsecond radio astrometry.

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Section: Galactic Structurementioning

confidence: 99%

Microarcsecond Radio Astrometry

Reid

Honma

2014

Annu. Rev. Astron. Astrophys.

177

191

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“…: LAMOST Fellow Precise distance is of paramount importance for tracing the structure of the Galactic spiral arms. The accurate distance measurements of masers from the Very Long Baseline Interferometry (VLBI) have been vital to disentangle the spiral arms, spurs and arm branches (Xu et al 2006;Honma et al 2007;Reid et al 2014). However, there are accurate trigonometric parallax observations for only about 100 masers, mostly in the first and second quadrants of the disk.…”

Section: Introductionmentioning

confidence: 99%

The Galactic spiral structure as revealed by O- and early B-type stars

Chen

Huang

Hou

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We investigate the morphology and kinematics of the Galactic spiral structure based on a new sample of O-and early B-type stars. We select 6,858 highly confident OB star candidates from the combined data of the VST Photometric Hα Survey Data Release 2 (VPHAS+ DR2) and the Gaia Data Release 2 (Gaia DR2). Together with the O-B2 stars from the literature, we build a sample consisting of 14,880 O-and early B-type stars, all with Gaia parallax uncertainties smaller than 20 per cent. The new sample, hitherto the largest one of O-and early B-type stars with robust distance and proper motion estimates, covers the Galactic plane of distances up to " 6 kpc from the Sun. The sample allows us to examine the morphology of the Scutum, Sagittarius, Local and Perseus Arms in great detail. The spiral structure of the Milky Way as traced by O-and early B-type stars shows flocculent patterns. Accurate structure parameters, as well as the means and dispersions of the vertical velocity distributions of the individual spiral arms are presented.

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“…Such work, augmented by radio wavelength data, was extended to cover most of the Galaxy by Georgelin & Georgelin (1976) and Russeil (2003). In the last decade, Very Long Baseline Interferometry (VLBI) at centimeter wavelengths has provided hundreds of parallaxes to very young, massive stars with accuracies often as good as ±0.01 mas (Xu et al 2006;Xu et al 2016;Honma et al 2007;Reid et al 2014), substantially increasing our knowledge of the spiral arms in our Galaxy. Recent VLBI parallaxes, however, have mostly been limited to stars visible from the northern hemisphere, leaving the fourth Galactic quadrant largely unexplored.…”

Section: Introductionmentioning

confidence: 99%

A comparison of the local spiral structure from Gaia DR2 and VLBI maser parallaxes

Bian

Reid

et al. 2018

A&A

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Context. The Gaia mission has released the second data set (Gaia DR2), which contains parallaxes and proper motions for a large number of massive, young stars. Aims. We investigate the spiral structure in the solar neighborhood revealed by Gaia DR2 and compare it with that depicted by VLBI maser parallaxes. Methods. We examined three samples with different constraints on parallax uncertainty and distance errors and stellar spectral types:(1) all OB stars with parallax errors of less than 10%; (2) only O-type stars with 0.1 mas errors imposed and with parallax distance errors of less than 0.2 kpc; and (3) only O-type stars with 0.05 mas errors imposed and with parallax distance errors of less than 0.3 kpc.Results. In spite of the significant distance uncertainties for stars in DR2 beyond 1.4 kpc, the spiral structure in the solar neighborhood demonstrated by Gaia agrees well with that illustrated by VLBI maser results. The O-type stars available from DR2 extend the spiral arm models determined from VLBI maser parallaxes into the fourth Galactic quadrant, and suggest the existence of a new spur between the Local and Sagittarius arms.

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Astrometry of Galactic Star-Forming Region Sharpless 269 with VERA: Parallax Measurements and Constraint on Outer Rotation Curve

Cited by 124 publications

References 29 publications

Microarcsecond Radio Astrometry

Microarcsecond Radio Astrometry

The Galactic spiral structure as revealed by O- and early B-type stars

A comparison of the local spiral structure from Gaia DR2 and VLBI maser parallaxes

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