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Sandström, Karin; Peek, J. E. G.; Bower, Geoffrey C.; Bolatto, Alberto D.; Plambeck, R. L.

doi:10.1086/520922

Cited by 139 publications

(58 citation statements)

References 37 publications

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“…For example, the distance to the Orion Nebula, determined by a number of trigonometric parallax measurements using radio continuum emission from stars in its associated cluster Sandstrom et al 2007), water masers , and SiO masers (Kim et al 2008), turned out to be 10% less than previously assumed, resulting in 10% lower masses, 20% fainter luminosities, and 20-30% younger ages for the stars in the cluster.…”

Section: Introductionmentioning

confidence: 92%

Trigonometric parallaxes of 6.7 GHz methanol masers

Rygl

Brunthaler

Reid³

et al. 2010

A&A

153

131

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Aims. Emission from the 6.7 GHz methanol maser transition is very strong, is relatively stable, has small internal motions, and is observed toward numerous massive star-forming regions in the Galaxy. Our goal is to perform high-precision astrometry using this maser transition to obtain accurate distances to their host regions. −0.06 kpc for S 255. The distances and proper motions yield the full space motions of the star-forming regions hosting the masers, and we find that these regions lag circular rotation on average by ∼17 km s −1 , a value comparable to those found recently by similar studies.

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Section: Introductionmentioning

confidence: 92%

Trigonometric parallaxes of 6.7 GHz methanol masers

Rygl

Brunthaler

Reid³

et al. 2010

A&A

153

131

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“…In contrast to Reid et al (2009), McMillan & Binney (2010 show that it is fairly justified to adopt their corresponding circular velocity components as probes for the Galactic rotation curve when taking the Schönrich et al values for the peculiar motion of the Sun. Following this argument, parallaxes, proper motions, and heliocentric radial velocities for 30 maser sources have been compiled from the literature (Sandstrom et al 2007;Hirota et al 2008a,b;Reid et al 2009;Rygl et al 2010;Sato et al 2010;Asaki et al 2010;Niinuma et al 2011;Honma et al 2011). To account for the virial motion of the masers with respect to their high-mass star-forming regions, a constant uncertainty of 7 km s −1 (see Reid et al 2009) is added in quadrature to the measurement errors when computing circular velocities.…”

Section: Rotation Curvementioning

confidence: 99%

Milky Way mass models for orbit calculations

Irrgang

Wilcox

Tucker

et al. 2013

A&A

226

339

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Context. Studying the trajectories of objects like stars, globular clusters, or satellite galaxies in the Milky Way allows the dark matter halo to be traced but requires reliable models of its gravitational potential. Aims. Realistic, yet simple and fully analytical, models have already been presented in the past. However, improved, as well as new, observational constraints have become available in the meantime, calling for a recalibration of the respective model parameters. Methods. Three widely used model potentials are revisited. By a simultaneous least-squares fit to the observed rotation curve, in-plane proper motion of Sgr A*, local mass/surface density, and the velocity dispersion in Baade's window, parameters of the potentials are brought up-to-date. The mass at large radii -in particular, that of the dark matter halo -is hereby constrained by requiring that the most extreme known halo, blue horizontal-branch star has to be bound to the Milky Way. Results. The Galactic mass models are tuned to yield a very good match to recent observations. The mass of the dark matter halo is -within the limitations of the applied models -estimated in a fully consistent way. As a first application, the trajectory of the hypervelocity star HE 0437-5439 is investigated again to check its suggested origin in the Large Magellanic Cloud (LMC). Conclusions. Despite their simplicity, the presented Milky Way mass models are very able to reproduce all observational constraints. Their analytical and simple form makes them ideally suited for fast and accurate orbit calculations. The LMC cannot be ruled out as HE 0437-5439's birthplace.

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“…As in the case of Vela, the superposition of all the associations and clusters of the Orion stream in the line of sight (Fig. 7) has led to great confusion regarding the distances and ages of the stellar groups belonging to the Orion OB1 complex (Genzel et al 1981;Brown et al 1994;Hirota et al 2007;Sandstrom et al 2007;Jeffries 2007;Lombardi et al 2011;Alves & Bouy 2012;Bouy et al 2014). Given that it might be one of the richest OB associations closest to Earth, follow-up observations to find its members and characterize its properties are very much needed.…”

Section: Orion Blue Stream: the Forest In Front Of The Treementioning

confidence: 99%

Cosmography of OB stars in the solar neighbourhood

Bouy

Alves

2015

A&A

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We construct a 3D map of the spatial density of OB stars within 500 pc from the Sun using the Hipparcos catalogue and find three large-scale stream-like structures that allow a new view on the solar neighbourhood. The spatial coherence of these blue streams and the monotonic age sequence over hundreds of parsecs suggest that they are made of young stars, similar to the young streams that are conspicuous in nearby spiral galaxies. The three streams are 1) the Scorpius to Canis Majoris stream, covering 350 pc and 65 Myr of star formation history; 2) the Vela stream, encompassing at least 150 pc and 25 Myr of star formation history; and 3) the Orion stream, including not only the well-known Orion OB1abcd associations, but also a large previously unreported foreground stellar group lying only 200 pc from the Sun. The map also reveals a remarkable and previously unknown nearby OB association, between the Orion stream and the Taurus molecular clouds, which might be responsible for the observed structure and star formation activity in this cloud complex. This new association also appears to be the birthplace of Betelgeuse, as indicated by the proximity and velocity of the red giant. If this is confirmed, it would solve the long-standing puzzle of the origin of Betelgeuse. The well-known nearby star-forming low-mass clouds, including the nearby T and R associations Lupus, Cha, Oph, CrA, Taurus, Vela R1, and various low-mass cometary clouds in Vela and Orion, appear in this new view of the local neighbourhood to be secondary star formation episodes that most likely were triggered by the feedback from the massive stars in the streams. We also recover well-known star clusters of various ages that are currently cruising through the solar neighbourhood. Finally, we find no evidence of an elliptical structure such as the Gould belt, a structure we suggest is a 2D projection effect, and not a physical ring.

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Cited by 139 publications

References 37 publications

Trigonometric parallaxes of 6.7 GHz methanol masers

Trigonometric parallaxes of 6.7 GHz methanol masers

Milky Way mass models for orbit calculations

Cosmography of OB stars in the solar neighbourhood

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