Molecular Gas in the NGC 6334 Star Formation Region

1999 ◽  
Vol 124 (2) ◽  
pp. 439-463 ◽  
Author(s):  
Kathleen E. Kraemer ◽  
James M. Jackson
Keyword(s):  
Star Formation ◽  
Molecular Gas ◽  
Star Formation Region ◽  
Formation Region ◽  
Ngc 6334

scholarly journals Subarcsecond Near-Infrared Images of Massive Star Formation Region NGC 6334 V

2007 ◽  
Vol 59 (1) ◽  
pp. 221-225 ◽  
Author(s):  
Jun Hashimoto ◽  
Motohide Tamura ◽  
Hiroshi Suto ◽  
Lyu Abe ◽  
Miki Ishii ◽  
...  
Keyword(s):  
Star Formation ◽  
Massive Star ◽  
Near Infrared ◽  
Infrared Images ◽  
Massive Star Formation ◽  
Star Formation Region ◽  
Formation Region ◽  
Ngc 6334

scholarly journals Ammonia observations towards the Aquila Rift cloud complex

2020 ◽  
Vol 643 ◽  
pp. A178
Author(s):  
Kadirya Tursun ◽  
Jarken Esimbek ◽  
Christian Henkel ◽  
Xindi Tang ◽  
Gang Wu ◽  
...  
Keyword(s):  
Star Formation ◽  
Dust Emission ◽  
Turbulent Energy ◽  
Gravitational Energy ◽  
High Mass ◽  
Kinetic Temperature ◽  
Mass Star ◽  
Dense Gas ◽  
Star Formation Region ◽  
Formation Region

We surveyed the Aquila Rift complex including the Serpens South and W 40 regions in the NH3 (1,1) and (2,2) transitions making use of the Nanshan 26-m telescope. Our observations cover an area of ~ 1.5° × 2.2° (11.4 pc × 16.7 pc). The kinetic temperatures of the dense gas in the Aquila Rift complex obtained from NH3 (2,2)/(1,1) ratios range from 8.9 to 35.0 K with an average of 15.3 ± 6.1 K (errors are standard deviations of the mean). Low gas temperatures are associated with Serpens South ranging from 8.9 to 16.8 K with an average of 12.3 ± 1.7 K, while dense gas in the W 40 region shows higher temperatures ranging from 17.7 to 35.0 K with an average of 25.1 ± 4.9 K. A comparison of kinetic temperatures derived from para-NH3 (2,2)/(1,1) against HiGal dust temperatures indicates that the gas and dust temperatures are in agreement in the low-mass-star formation region of Serpens South. In the high-mass-star formation region W 40, the measured gas kinetic temperatures are higher than those of the dust. The turbulent component of the velocity dispersion of NH3 (1,1) is found to be positively correlated with the gas kinetic temperature, which indicates that the dense gas may be heated by dissipation of turbulent energy. For the fractional total-NH3 (para+ortho) abundance obtained by a comparison with Herschel infrared continuum data representing dust emission, we find values from 0.1 ×10−8 to 2.1 ×10−7 with an average of 6.9 (±4.5) × 10−8. Serpens South also shows a fractional total-NH3 (para+ortho) abundance ranging from 0.2 ×10−8 to 2.1 ×10−7 with an average of 8.6 (±3.8) × 10−8. In W 40, values are lower, between 0.1 and 4.3 ×10−8 with an average of 1.6 (±1.4) × 10−8. Weak velocity gradients demonstrate that the rotational energy is a negligible fraction of the gravitational energy. In W 40, gas and dust temperatures are not strongly dependent on the projected distance to the recently formed massive stars. Overall, the morphology of the mapped region is ring-like, with strong emission at lower and weak emission at higher Galactic longitudes. However, the presence of a physical connection between the two parts remains questionable.

A Survey of Emission-Line Stars in the CMa Star Formation Region

1986 ◽  
pp. 311-315
Author(s):  
Suhardja D. Wiramihardja ◽  
Tomokazu Kogure ◽  
Makoto Nakano ◽  
Shigeomi Yoshida ◽  
Ken’ichi Tatematsu
Keyword(s):  
Star Formation ◽  
Emission Line ◽  
Star Formation Region ◽  
Formation Region

scholarly journals A MID-INFRARED VIEW OF THE HIGH MASS STAR FORMATION REGION W51A

2016 ◽  
Vol 825 (1) ◽  
pp. 54 ◽  
Author(s):  
C. L. Barbosa ◽  
R. D. Blum ◽  
A. Damineli ◽  
P. S. Conti ◽  
D. M. Gusmão
Keyword(s):  
Star Formation ◽  
High Mass ◽  
Mass Star ◽  
Mid Infrared ◽  
Star Formation Region ◽  
Formation Region

scholarly journals Shock structure and shock heating in the Galactic central molecular zone

2013 ◽  
Vol 9 (S303) ◽  
pp. 104-105 ◽  
Author(s):  
Jürgen Ott ◽  
Michael Burton ◽  
Paul Jones ◽  
David S. Meier
Keyword(s):  
High Energy ◽  
Molecular Gas ◽  
Star Formation Region ◽  
Formation Region ◽  
Heating Source ◽  
Supermassive Black Hole ◽  
Shock Heating ◽  
Sgr A ◽  
Morphological Differences ◽  
High Energy Emission

AbstractWe present maps of a large number of dense molecular gas tracers across the central molecular zone of our Galaxy. The data were taken with the CSIRO/CASS Mopra telescope in Large Projects in the 1.3 cm, 7 mm, and 3 mm wavelength regimes. Here, we focus on the brightness of the shock tracers SiO and HNCO, molecules that are liberated from dust grains under strong (SiO) and weak (HNCO) shocks. The shocks may have occurred when the gas enters the bar regions and the shock differences could be due to differences in the moving cloud masses. Based on tracers of ionizing photons, it is unlikely that the morphological differences are due to selective photo-dissociation of the molecules. We also observe direct heating of molecular gas in strongly shocked zones, with high SiO/HNCO ratios, where temperatures are determined from the transitions of ammonia. Strong shocks appear to be the most efficient heating source of molecular gas, apart from high energy emission emitted by the central supermassive black hole Sgr A* and the processes within the extreme star formation region Sgr B2.

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