Desiderata for Future Work

Becker, W.; Contopoulos, G.

doi:10.1007/978-94-010-3275-9_86

Cited by 5 publications

(6 citation statements)

References 2 publications

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“…He pointed out that the distribution of OCs with the earliest spectral type between O and B2 probably followed three spiral arm segments in the vicinity of the Sun, and resembled the distribution of nearby HII regions, while the distribution of older OCs with spectral type between B3 and F did not indicate spiral arm segments and seemed to be random. These conclusions were confirmed by Becker & Fenkart (1970) and Fenkart & Binggeli (1979) with larger samples of OCs. With a sample of 212 OCs, Dias & Lépine (2005) showed that the OCs with ages up to about 1.2×10 7 yr remain in parts of the Perseus Arm, the Local Arm and the Sagittarius-Carina Arm; those with ages ∼20 Myr are leaving the spiral arms and filling the interarm regions; for clusters older than 30 Myr, the spiral or clumpy-like structure has disappeared in their distribution.…”

Section: Open Clusterssupporting

confidence: 60%

The spiral structure of the Milky Way

Hou

2018

Res. Astron. Astrophys.

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The morphology and kinematics of the spiral structure of the Milky Way are long-standing problems in astrophysics. In this review we firstly summarize various methods with different tracers used to solve this puzzle. The astrometry of Galactic sources is gradually alleviating this difficult situation caused mainly by large distance uncertainties, as we can currently obtain accurate parallaxes (a few µas) and proper motions (≈1 km s −1 ) by using Very Long Baseline Interferometry (VLBI). On the other hand, the Gaia mission is providing the largest, uniform sample of parallaxes for O-type stars in the entire Milky Way. Based upon the VLBI maser and Gaia O-star parallax measurements, nearby spiral structures of the Perseus, Local, Sagittarius and Scutum Arms are determined in unprecedented detail. Meanwhile, we estimate fundamental Galactic parameters of the distance to the Galactic center, R 0 , to be 8.35±0.18 kpc, and circular rotation speed at the Sun, Θ 0 , to be 240±10 km s −1 . We found kinematic differences between O stars and interstellar masers: the O stars, on average, rotate faster, >8 km s −1 than maser-traced high-mass star forming regions.

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Section: Open Clusterssupporting

confidence: 60%

The spiral structure of the Milky Way

Hou

2018

Res. Astron. Astrophys.

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“…Despite uncertainties in the distances to individual stars, it is clear that several of the stars we have observed are likely to be at considerable distances from the galactic center, well beyond the extended Perseus arm. Figure 4 shows the locations of the stars on the galactic plane relative to the spiral features described by Becker and Fenkart (1970), Henderson et al (1982, and the +II arm of Vogt and Moffat (1975). These diagrams are summarized in Elmegreen (1985).…”

Section: Discussionmentioning

confidence: 94%

Photometry of the Rubin Losee blue stars at the anticenter

Philip

Chromey

Dubois

1990

PASP

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“…The distance found in the previous section coupled with the galactic coordinates of the cluster (£ = 21?6, b = -0?8) show the cluster to be in the Carina-Sagittarius-Scutum arm of the Milky Way as identified by Becker and Fenkart (1970). I thank Dr. H. D. Abies for providing the electrographic UBV sequence in the cluster field and for the use of the observing facilities of the U.S.…”

Section: Discussionmentioning

confidence: 65%