scholarly journals Physical parameters of molecular clumps in the S254—S258 star formation region

2021 ◽  
Author(s):  
E. A. Popova ◽  
◽  
D. A. Ladeyschikov ◽  
M. S. Kirsanova ◽  
A. M. Sobolev ◽  
...  
Keyword(s):  
Star Formation ◽  
Optical Depth ◽  
Near Infrared ◽  
Continuum Emission ◽  
Physical Parameters ◽  
Star Formation Region ◽  
Formation Region ◽  
Molecular Lines ◽  
The Difference ◽  
Infrared Extinction

This research is focusing on studying of physical parameters in the S254—S258 star-formation complex. The following parameters were derived: column densities, clump masses, and highdensity tracers optical depth, including CS and HCO+ molecules. Different gas and dust tracers maps were used, including CO molecular lines, Bolocam 1.1 mm continuum emission and near-infrared extinction map. We also used the available CS and HCO+ data, which cover part of the S254-S258 region to make conclusions regarding the distribution of highdensity gas. The resulted values of physical parameters obtained through different tracers are slightly different. The discussion about the possible reason for the difference is provided.

scholarly journals The First Young Brown Dwarf in the Serpens Cloud

2003 ◽  
Vol 211 ◽  
pp. 83-86
Author(s):  
Jean-Louis Monin ◽  
Emmanuel Caux ◽  
Alain Klotz ◽  
Nicolas Lodieu
Keyword(s):  
Star Formation ◽  
Spectral Type ◽  
Near Infrared ◽  
Nir Spectroscopy ◽  
Brown Dwarfs ◽  
Brown Dwarf ◽  
Star Formation Region ◽  
Formation Region

We report the discovery of the first young brown dwarf in the Serpens cloud (BD-Ser 1). It is obscured by more than ten magnitudes of visual absorption as indicated by near infrared (NIR) photometric survey at the NTT and confirmed by NIR spectroscopy at the VLT. We estimate the mass of this brown dwarf to be M ~ 0.05 M⊙ and its age to be ~ 3.5 Myr. Available NIR indices in the literature (designed for field brown dwarfs) fail to provide its current spectral type but using a model they correctly determine its future spectral type to be T. This is the first young brown dwarf ever found deeply embedded in the Serpens star formation region

scholarly journals An optical and near-infrared exploration of the star formation region in Cygnus surrounding RNO 127

2003 ◽  
Vol 412 (1) ◽  
pp. 147-156 ◽  
Author(s):  
T. Movsessian ◽  
T. Khanzadyan ◽  
T. Magakian ◽  
M. D. Smith ◽  
E. Nikogosian
Keyword(s):  
Star Formation ◽  
Near Infrared ◽  
Star Formation Region ◽  
Formation Region

scholarly journals A wide-field near-infrared H22.122μm line survey of the Braid Nebula star formation region in Cygnus OB7

2012 ◽  
Vol 542 ◽  
pp. A111 ◽  
Author(s):  
T. Khanzadyan ◽  
C. J. Davis ◽  
C. Aspin ◽  
D. Froebrich ◽  
M. D. Smith ◽  
...  
Keyword(s):  
Star Formation ◽  
Near Infrared ◽  
Wide Field ◽  
Star Formation Region ◽  
Formation Region ◽  
Line Survey

A near-infrared study of the Monoceros R2 star formation region

1994 ◽  
Vol 425 ◽  
pp. 707 ◽  
Author(s):  
Eric M. Howard ◽  
Judith L. Pipher ◽  
William J. Forrest
Keyword(s):  
Star Formation ◽  
Near Infrared ◽  
Infrared Study ◽  
Star Formation Region ◽  
Formation Region

Near‐Infrared Imaging of the Star Formation Region AFGL 5142

2005 ◽  
Vol 629 (1) ◽  
pp. 288-298 ◽  
Author(s):  
Yafeng Chen ◽  
Yongqiang Yao ◽  
Ji Yang ◽  
Qin Zeng ◽  
Shuji Sato
Keyword(s):  
Star Formation ◽  
Near Infrared ◽  
Infrared Imaging ◽  
Near Infrared Imaging ◽  
Star Formation Region ◽  
Formation Region

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.

Sign in / Sign up

Export Citation Format

Share Document