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

Chen, Bingqiu; Huang, Yang; Hou, Li‐Peng; Tian, Hao; Li, G. X.; Yuan, Haibo; Wang, H. F.; Wang, C.; Tian, Zhijia; Liu, X. W.

doi:10.1093/mnras/stz1357

Cited by 52 publications

(52 citation statements)

References 42 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…The green, pink and blue dashed lines mark respectively a possible spur 'Lower Sagittarius-Carina Spur', the 'split' found by Lallement et al (2019) and the spur identified by Xu et al (2016). Three black dashed circles mark the positions of three possible hole patterns in the Sagittarius and Perseus Arms identified in Chen et al (2019a). The Sun, assumed to be at the position of (X, Y, Z) = (´8.34, 0, 0) kpc, is located at the centre of the plot.…”

Section: Comparison With Previous Workmentioning

confidence: 88%

“…A significant fraction of the clouds concentrated in the direction of the Galactic anti-centre (l " 180˝), where the masers and OB stars also clump. Although several molecular clouds are visible in the two 'holes' repoted by Chen et al (2019a), the 'holes' are less populated by the clouds than in other areas.…”

Section: The Galactic Spiral Structure As Traced By the Molecular Cloudsmentioning

confidence: 93%

“…The good agreement validates the robustness of methods used in both papers. Chen et al (2019a). Circles of the aforementioned colours are the masers from Xu et al (2018) that are probably associated with the individual Arms.…”

Section: Comparison With Previous Workmentioning

confidence: 93%

“…Circles of the aforementioned colours are the masers from Xu et al (2018) that are probably associated with the individual Arms. The grey background image represents the spatial distribution of the OB stars from Chen et al (2019a). The green, pink and blue dashed lines mark respectively a possible spur 'Lower Sagittarius-Carina Spur', the 'split' found by Lallement et al (2019) and the spur identified by Xu et al (2016).…”

Section: Comparison With Previous Workmentioning

confidence: 96%

“…The Perseus Arm is quite a diffuse arm. Based on the spatial distribution of the OB stars and masers, Chen et al (2019a) identify two possible 'hole' patterns within the Arm with no masers and few OB stars. The molecular clouds identified here around the two 'holes' are also fragmented, albeit with a different pattern.…”

Section: The Galactic Spiral Structure As Traced By the Molecular Cloudsmentioning

confidence: 99%

See 4 more Smart Citations

A large catalogue of molecular clouds with accurate distances within 4 kpc of the Galactic disc

Chen

Yuan

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We present a large, homogeneous catalogue of molecular clouds within 4 kpc from the Sun at low Galactic latitudes (|b| ă 10˝) with unprecedented accurate distance determinations. Based on the three-dimensional dust reddening map and estimates of colour excesses and distances of over 32 million stars presented in Chen et al, we have identified 567 dust/molecular clouds with a hierarchical structure identification method and obtained their distance estimates by a dust model fitting algorithm. The typical distance uncertainty is less than 5 per cent. As far as we know, this is the first large catalogue of molecular clouds in the Galactic plane with distances derived in a direct manner. The clouds are seen to lie along the Sagittarius, Local and Perseus Arms. In addition to the known structures, we propose the existence of a possible spur, with a pitch angle of about 34˝, connecting the Local and the Sagittarius Arms in the fourth quadrant. We have also derived the physical properties of those molecular clouds. The distribution of cloud properties in different parameter spaces agrees grossly with the previous results. Our cloud sample is an ideal starting point to study the concentration of dust and gas in the solar vicinity and their star formation activities.

show abstract

Section: Comparison With Previous Workmentioning

confidence: 88%

Section: The Galactic Spiral Structure As Traced By the Molecular Cloudsmentioning

confidence: 93%

Section: Comparison With Previous Workmentioning

confidence: 93%

Section: Comparison With Previous Workmentioning

confidence: 96%

Section: The Galactic Spiral Structure As Traced By the Molecular Cloudsmentioning

confidence: 99%

See 3 more Smart Citations

A large catalogue of molecular clouds with accurate distances within 4 kpc of the Galactic disc

Chen

Yuan

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

FEDReD

Hottier

Babusiaux

Arenou

2020

A&A

View full text Add to dashboard Cite

Aims. We aim to map the 3D distribution of the interstellar extinction of the Milky Way disc up to distances larger than those probed with the Gaia parallax alone. Methods. We applied the FEDReD (Field Extinction-Distance Relation Deconvolver) algorithm to the 2MASS near-infrared photometry together with the Gaia DR2 astrometry and photometry. This algorithm uses a Bayesian deconvolution approach, based on an empirical HR-diagram representative of the local thin disc, in order to map the extinction as a function of distance of various fields of view. Results. We analysed more than 5.6 million stars to obtain an extinction map of the entire Galactic disc within |b| < 0.24°. This map provides information up to 5 kpc in the direction of the Galactic centre and more than 7 kpc in the direction of the anticentre. This map reveals the complete shape of structures that are known locally, such as the Vela complex and the split of the local arm. Furthermore, our extinction map shows many large “clean bubbles”, especially the one in the Sagittarius-Carina complex, and four others, which define a structure that we nickname the butterfly.

show abstract

OB stars and YSO populations in the region of NGC 6334–NGC 6357 as seen withGaiaDR2

Russeil

Zavagno

Nguyen

et al. 2020

A&A

View full text Add to dashboard Cite

Aims. Our goal is to better understand the origin and the star-formation history of regions NGC 6334 and NGC 6357. We focus our study on the kinematics of young stars (young stellar objects and OB stars) in both regions mainly on the basis of the Gaia DR2 data. Methods. For both regions, we compiled catalogs of OB stars and young stellar objects from the literature and complemented them using VPHAS+ DR2 and Spitzer IRAC/GLIMPSE photometry catalogues. We applied a cross-match with the Gaia DR2 catalog to obtain information on the parallax and transverse motion. Results. We confirm that NGC 6334 and NGC 6357 are in the far side of the Saggitarius-Carina arm at a distance of 1.76 kpc. For NGC 6357, OB stars show strong clustering and ordered star motion with Vlon ∼–10.7 km s−1 and Vlat ∼3.7 km s−1, whereas for NGC 6334, no significant systemic motion was observed. The OB stars motions and distribution in NGC 6334 suggest that it should be classified as an association. Ten runaway candidates may be related to NGC 6357 and two to NGC 6334, respectively. The spatial distributions of the runaway candidates in and around NGC 6357 favor a dynamical (and early) ejection during the cluster(s) formation. Because such stars are likely to be ejected during a cluster’s formation, the fact that not as many such stars are observed towards NGC 6334 suggests different formation conditions than have been assumed for NGC 6357.

show abstract

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

Cited by 52 publications

References 42 publications

A large catalogue of molecular clouds with accurate distances within 4 kpc of the Galactic disc

A large catalogue of molecular clouds with accurate distances within 4 kpc of the Galactic disc

FEDReD

OB stars and YSO populations in the region of NGC 6334–NGC 6357 as seen withGaiaDR2

Contact Info

Product

Resources

About