A deep H$\mathsf{\alpha}$ survey of the Milky Way

Russeil, D.; Adami, C.; Amram, P.; Coarer, E. Le; Georgelin, Y. P.; Marcelin, M.; Parker, Quentin A.

doi:10.1051/0004-6361:20048090

Cited by 25 publications

(34 citation statements)

References 32 publications

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“…In addition, in Hα, the local component, located around 200 pc (see, e.g. Russeil et al 2005), is expected to have a velocity of −5 km s −1 , which is also similar to the mean velocity of NGC 6334 and NGC 6357, which are located farther away.…”

Section: General Aspectsmentioning

confidence: 91%

NGC 6334 and NGC 6357: Hαkinematics and the nature of the H II regions

Russeil

Tigé

Adami

et al. 2016

A&A

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Aims. NGC 6334 and NGC 6357 are amongst the most active, optically visible Galactic star-forming complexes. They are composed of several H ii regions that have a significant impact on their surrounding. The aim of this paper is to present a kinematic study of the optical H ii regions that belong to NGC 6334 and NGC 6357.Methods. We use Fabry-Perot interferometer observations of the Hα line, which cover NGC 6334 and NGC 6357. These observations allow us to analyse the Hα line profiles to probe the kinematics of the ionised gas of both regions. We complement the Hα observations with multi-wavelength data to specify the nature of the H ii regions. Results. We determine the dynamical nature of the optical H ii regions that belongs to NGC 6334 and NGC 6357. In NGC 6334, GUM 61 is an expanding wind shell-like H ii region, GUM 64b exhibits a champagne flow, GM1-24 is the Hα counterpart of two larger regions and H ii 351.2+0.5 is, in fact, composed of two H ii regions. In NGC 6357, H ii 353.08+0.28 and H ii 353.09+0.63 are probably stellar wind-shaped bubble H ii regions, while H ii 353.42+0.45 is a classical photo-ionised H ii region. We suggest that, at large scale, star-formation seems to be triggered where large/old H ii regions intersect. Inversely, stellar formation seems to have already started in the NGC 6334 north-east filament, irrespective of any evident external H ii region impact. While NGC 6357 shows more complicated kinematics, NGC 6334 is characterised by a more active stellar formation.

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Section: General Aspectsmentioning

confidence: 91%

NGC 6334 and NGC 6357: Hαkinematics and the nature of the H II regions

Russeil

Tigé

Adami

et al. 2016

A&A

Self Cite

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“…The GMC known as G333 hosts at least four highly obscured MYSCs (Figuerêdo et al 2005;Bains et al 2006) plus the slightly more revealed, multi-clustered star-forming complex RCW 106 (Russeil et al 2005). G333 has a conspicuously elongated morphology, extending over 80 pc along the Galactic Plane but with a width of only ∼15 pc.…”

Section: G3336−02mentioning

confidence: 99%

The Massive Star-Forming Regions Omnibus X-Ray Catalog

Townsley

Broos

Garmire

et al. 2014

ApJS

150

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We present the Massive Star-forming Regions (MSFRs) Omnibus X-ray Catalog (MOXC), a compendium of X-ray point sources from Chandra/ACIS observations of a selection of MSFRs across the Galaxy, plus 30 Doradus in the Large Magellanic Cloud. MOXC consists of 20,623 X-ray point sources from 12 MSFRs with distances ranging from 1.7 kpc to 50 kpc. Additionally, we show the morphology of the unresolved X-ray emission that remains after the cataloged X-ray point sources are excised from the ACIS data, in the context of Spitzer and WISE observations that trace the bubbles, ionization fronts, and photon-dominated regions that characterize MSFRs. In previous work, we have found that this unresolved X-ray emission is dominated by hot plasma from massive star wind shocks. This diffuse X-ray emission is found in every MOXC MSFR, clearly demonstrating that massive star feedback (and the several-million-degree plasmas that it generates) is an integral component of MSFR physics.

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“…Russeil et al (2005) obtained a deep H study of the Milky Way near longitude 332 and found proper distance estimates for several optical H ii regions. They fitted many layers, each one at a different radial velocity and kinematic distance, and identified each with a spiral arm or another large object (association, supernova, cloud complex); they found the SagittariusCarina arm at À24 km s À1 and 1.9 kpc, etc.…”

Section: Evaluation and Weightingmentioning

confidence: 99%

The Spiral Arms and Interarm Separation of the Milky Way: An Updated Statistical Study

2005

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Measurements of the spiral arms (their pitch angle, number, shape, and the interarm separation) in the Milky Way have been published in the period from 1980 to early 2005, using different methods that yielded slightly or widely differing values, depending on hidden or unknown biases. A meta-analysis would be useful for searching for trends among these individual studies. First, we find a convergence for three parameters: the pitch angle, the number of arms, and the shape of the arms. Second, we find a change for the interarm separation near the Sun, a decrease of about 25%; it is our determination of these parameters that evolves, not the actual physical arms. Third, we recalibrate a recent arm model to take account of that gradual change and compare it with the spread in each arm parameter.

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A deep H$\mathsf{\alpha}$ survey of the Milky Way

Cited by 25 publications

References 32 publications

NGC 6334 and NGC 6357: Hαkinematics and the nature of the H II regions

NGC 6334 and NGC 6357: Hαkinematics and the nature of the H II regions

The Massive Star-Forming Regions Omnibus X-Ray Catalog

The Spiral Arms and Interarm Separation of the Milky Way: An Updated Statistical Study

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