Table 1
Characteristics of the regions in NGC 6334 and NGC 6357.
| Radio | Size | V exp | V sys a | SpIa | Regiona | σ vel | σ | 8 μm featuresa |
| Ident. | “×” | km s-1 | km s-1 | km s-1 | km s-1 | |||
|
|
||||||||
| NGC 6357 | ||||||||
|
|
||||||||
| G353.43+0.46 | 3.0 × 3.17 | 1.6 | −5 | +0.9 (+0.49) | H ii 353.42+0.45 | 2.06 | 8.87 | Faint emission, rims, nascent pillars |
| G353.27+0.59 | 5.83 × 5.67 | ≥5 | 2.5 | +0.3 | H ii 353.24+0.60 | 1.04 | 3.72 | Strong emission, broken ring, pillars, known as CS59h |
| G353.19+0.90 | 1.83 × 2.00 | 16.6 | −4.7 | −0.5 (−0.05) | – | – | – | Semi-ring emanating from the bright rim facing Pismis 24 |
| G353.19+0.84 | 0.58 × 0.67 | 1.2 | −14.5 | −0.4 | – | – | – | Pillar, nascent pillar and birght rims |
| G353.13+0.65b | 0.73 × 1.40 | – | −4 | −0.8 | – | – | – | Thin and patchy filaments, at the edge of G353.08+0.63 |
| G353.10+0.60b | 0.75 × 0.66 | – | −4 | +0.8 | – | – | – | no 8 μm |
| G353.09+0.66b | 1.25 × 0.83 | – | −4 | −0.4 | – | – | – | Thin and patchy filaments, edge of G353.08+0.63 |
| G353.08+0.63b | 4.50 × 4.33 | 18 | −4 | +0.3 | H ii 353.09+0.63 | 1.23 | 3.57 | Strong emission, group of bubbles, pillars, known as CS63h |
| G353.07+0.31 | 5.32 × 6.32 | 8 | −3 | +0.6/−0.4 (+0.06) | H ii 353.08+0.28 | 3.32 | 10.67 | Semi-ring, pillars, rims, associated to CS62h |
|
|
||||||||
| NGC 6334 | ||||||||
|
|
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| G351.69+0.67 | 1.83 × 1.83 | – | 3.1 | +1.2 | – | – | Semi-ring, nascent pillar, known as CS78h | |
| G351.68+0.61 | 1.54 × 1.54 | – | – | -0.7 | H ii 351.67+0.62f | – | – | Diffuse emission with no structure |
| G351.65+0.51 | 2.83 × 2.83 | – | −2.9 | +0.7 | H ii 351.64+0.51f | – | – | Closed floculent ring, known as CS79h |
| G351.42+0.67 | 0.54 × 0.50 | – | −8 | −0.8 | NGC 6334-E | – | – | Compact patchy emission |
| G351.41+0.64 | 0.34 × 0.34 | – | −6.9 | – | NGC 6334-I | – | – | Compact patchy emission |
| G351.38+0.74 | 1.83 × 1.50 | 17.7 | −3.6 | −0.4 | GUM 64c | – | – | Irregular emission |
| G351.36+1.01d | 1.98 × 3.40 | – | −8.6 | (1.06) | – | – | – | |
| G351.36+0.65 | 1.18 × 1.00 | 14 | −5 | −0.7 | NGC 6334-D | – | – | Filled ring, known as CS85h |
| G351.33+0.61 | 0.33 × 0.33 | – | −6 | −0.08 | NGC 6334-DS | – | – | Semi-ring, central compact source |
| G351.32+0.73 | 1.17 × 1.00 | – | −8 | −0.5 (−0.52) | GUM 64c | 1.19 | 7.93 | Group of 3 pillars |
| 6.19 × 5.53 | ≥6 | −5 | – | GUM 64b (351.32+0.61) | 2.49 | 7.62 | Irregular emission, include the small closed ring CS85h | |
| G351.31+0.66 | 0.82 × 0.63 | 14 | −8 | −0.3 | – | – | – | Core-halo feature |
| G351.27+0.67 | 0.30 × 0.30 | – | – | – | – | – | – | Semi-ring feature |
| G351.26+1.02d | 2.67 × 1.90 | – | −3.6 | – | – | – | – | Closed ring, known as CS87h |
| G351.24+0.66 | 0.99 × 0.42 | 15.7 | −0.2 | −1.2 | NGC 6334-A | – | – | Bipolar morphology, known as CS88h |
| G351.17+0.70 | 1.95 × 2.19 | 16.5 | −7 | −0.9 | GUM 64a | – | – | Irregular, brigth rim, known as CS89h |
| G351.15+0.49 | 4.43×4.37 | 10 | −10 | +0.06c (+0.85) | H ii 351.2+0.5=GUM 62 | 2.11 | 5.63 | Faint diffuse broken ring, brigth rim, include the closed ring CS90h |
| G350.99+0.65 | 6.06 × 4.31 | 23 | −9 | −0.6 (+1.97) | GUM 61 | 12.21 | 12.15 | Broken ring, strong emission, brigth rims, known as CS94h |
| G350.50+0.95e | 1.32 × 0.90 | 6.6 | −10 | −0.7/+0.3e (−0.60) | GM 1-24 | 2.11 | 6.66 | |
Notes.
The Vsys is either the radio-recombination line (Anderson et al. 2011; Caswell & Haynes 1987) or the Hα velocity. Column 5 gives the mean spectral index. The spectral index calculated between 8.35 GHz and 14.35 GHz by Langston et al. (2000) is given into parenthesis. Column 6 gives the other region’s name and/or the galactic coordinates of the optical counterpart of the radio region. Column 11 gives 8 μm notes for optical H ii regions only.
The regions G353.13+0.65, G353.10+0.60 and G353.09+0.66 are compact radio sources on the border of the larger and optically visible region G353.08+0.63.
Radio sources not identified on radio maps but taken from Anderson et al. (2011).
G350.50+0.95 is a compact radio source located inside GM1-24 which is the more extended Hα emission. The spectral index is negative towards the compact radio source but positive in the more diffuse part of the region.
These regions are seen in Hα but they have not been observed with the Fabry-Perot interferometer.
From Churchwell et al. 2007 catalog.
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