The spiral structure of the Galaxy revealed by CS sources and evidence for the 4:1 resonance

@article{Lpine2010TheSS,
  title={The spiral structure of the Galaxy revealed by CS sources and evidence for the 4:1 resonance},
  author={Jacques R. D. L{\'e}pine and Alexandre Roman-Lopes and Zulema Abraham and Thiago C. Junqueira and Yu. N. Mishurov},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2010},
  volume={414},
  pages={1607-1616}
}
We present a map of the spiral structure of the Galaxy, as traced by molecular carbon monosulphide (CS) emission associated with IRAS sources which are believed to be compact H ii regions. The CS line velocities are used to determine the kinematic distances of the sources in order to investigate their distribution in the galactic plane. This allows us to use 870 objects to trace the arms, a number larger than that of previous studies based on classical H ii regions. The distance ambiguity of… 

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References

SHOWING 1-10 OF 50 REFERENCES

Star-forming complexes and the spiral structure of our Galaxy

We have carried out a multiwavelength study of the plane of our Galaxy in order to establish a star-forming-complex catalogue which is as complete as possible. Features observed include H, H109, CO,

Spiral Structure in the Outer Galactic Disk. I. The Third Galactic Quadrant

We combine optical and radio observations to trace the spiral structure in the third quadrant of the Milky Way. The optical observations consist of a large sample of young open clusters and

Direct Determination of the Spiral Pattern Rotation Speed of the Galaxy

The rotation velocity of the spiral pattern of the Galaxy is determined by direct observation of the birthplaces of open clusters of stars in the Galactic disk as a function of their age. Our

The spiral structure of our Milky Way Galaxy

Context. The spiral structure of our Milky Way Galaxy is not yet known. HII regions and giant molecular clouds are the most prominent spiral tracers. Models with 2−4 arms have been proposed to

Spatial distribution of Galactic Hii regions

We present a new, detailed, analysis of the spatial distribution of Galactic H II regions, exploiting a far richer data base than used in previous analyses. Galactocentric distances have been derived

Statistics of young starforming complexes in spiral galaxies using NIR photometry

Aims. Very young stellar clusters and cluster complexes may be embedded in dust lanes along spiral arms in disk galaxies and escape detection in visual bands. Observations in the near-infrared K-band

A new model for the infrared brightness of the Galaxy

We present a model that reproduces the near-infrared brightness distribution of the Galaxy, and we compare its predictions with the results of the Spacelab observations obtained by Kent et al. and

Kinematics of young stars. II. Galactic spiral structure

The young star velocity eld is analysed by means of a galactic model which takes into account solar motion, dierential galactic rotation and spiral arm kinematics. We use two samples of Hipparcos

Globular Cluster System and Milky Way Properties Revisited

Aims. Updated data of the 153 Galactic globular clusters are used to readdress fundamental parameters of the Milky Way, such as the distance of the Sun to the Galactic centre, the bulge and halo

The distance to the center of the Galaxy

For nearly a century astronomers have expended considerable effort to determine the size of the Milky Way. This effort is worthwhile because any change in the value of the distance from the Sun to