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

scholarly journals A young binary brown dwarf in the R-CrA star formation region

2004 ◽  
Vol 424 (1) ◽  
pp. 213-226 ◽  
Author(s):  
H. Bouy ◽  
W. Brandner ◽  
E. L. Martín ◽  
X. Delfosse ◽  
F. Allard ◽  
...  
Keyword(s):  
Star Formation ◽  
Brown Dwarf ◽  
Star Formation Region ◽  
Formation Region

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 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 A Deep Large area Search for Low Luminosity Stars

1998 ◽  
Vol 11 (1) ◽  
pp. 435-435
Author(s):  
Hugh R.A. Jones ◽  
Mike R.S. Hawkins
Keyword(s):  
Spectral Type ◽  
Low Temperatures ◽  
Current Model ◽  
Brown Dwarfs ◽  
Evolutionary Models ◽  
Spectral Indices ◽  
Late Type ◽  
Brown Dwarf ◽  
Large Area ◽  
M Dwarfs

In a recent survey for faint red stars from a digital stack of Schmidt plates a number of candidate objects were identified. Parallax’s for three of these objects have been reported showing them to have luminosities which interpreted within the available evolutionary models indicate them to be good brown dwarf candidates. Here we examine spectra of these objects and others from the plate stack. Using standard spectral indices we find that for a given spectral type their spectra are more consistent with the Pleiades brown dwarfs (PPL 15, Teide 1 and Calar 3) than with standard late-type M dwarfs. Our interpretation is that this is due to their selection by RF IN colours which at values > 3 preferentially selects objects with relatively low gravities. For late-type M dwarfs and brown dwarfs low gravities are expected to be a reliable indication of youth. We also notice that the stack objects generally have strong FeH absorption for their spectral type. Current model atmospheres suggest that FeH strongly increases in strength toward lower metallicities and lower temperatures. We believe that this is not consistent with the available observational evidence from late-type M dwarfs. It is possible that solid Fe is forming inthe low temperature atmospheres relatively depleting FeH strengths toward lower temperatures. We find some evidence that for dwarfs at low temperatures dust formation is less prevalent in lower gravity objects suggesting that dwarfs at low temperatures stronger FeH may be an indication of youth. In addition to the spectral evidence the three stack objects whose parallax’s have been measured show small tangential velocities which is a further indication of youth.

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