Lynds Bright Nebulae: Sites of possible twisted filaments and ongoing star formation. (arXiv:2107.10247v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dewangan_L/0/1/0/all/0/1">L. K. Dewangan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dhanya_J/0/1/0/all/0/1">J. S. Dhanya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhadari_N/0/1/0/all/0/1">N. K. Bhadari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ojha_D/0/1/0/all/0/1">D. K. Ojha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baug_T/0/1/0/all/0/1">T. Baug</a>
The paper presents an analysis of multi-wavelength data of two Lynds Bright
Nebulae (LBN), LBN 140.07+01.64 and LBN 140.77$-$1.42. The 1420 MHz continuum
map reveals an extended Y-shaped feature (linear extent ~3.7 deg), which
consists of a linear part and a V-like structure. The sites LBN 140.07+01.64
and AFGL 437 are located toward the opposite sides of the V-like structure, and
LBN 140.77$-$1.42 is spatially seen toward the linear part. Infrared-excess
sources are traced toward the entire Y-feature, suggesting star formation
activities. Infrared and sub-millimeter images show the presence of at least
two large-scale dust filaments extended toward the LBN sources. The Herschel
maps, which are available only toward the northern and central parts of the
Y-feature, display the presence of higher column density (> 2.4 X 10^{21}
cm^{-2}) of materials toward the filaments. Using the 12CO(1-0) line data, the
distribution of molecular gas at [-42.7, -34.4] km/s traces the cloud
associated with the Y-feature, and confirms the existence of filaments. The
large-scale filaments appear to be possibly spatially twisted. There is a hint
of an oscillatory-like velocity pattern along both the filaments, favouring
their proposed twisted nature. It is the first study showing the possible
twisting of filaments, which is more prominent in the northern and central
parts of the Y-feature. This possible twisting/coupling of the large-scale
filaments appears to be responsible for the observed star formation (including
known OB-stars). The proposed physical process and the energetics of OB-stars
together seem to explain the origin of the ionized Y-feature.
The paper presents an analysis of multi-wavelength data of two Lynds Bright
Nebulae (LBN), LBN 140.07+01.64 and LBN 140.77$-$1.42. The 1420 MHz continuum
map reveals an extended Y-shaped feature (linear extent ~3.7 deg), which
consists of a linear part and a V-like structure. The sites LBN 140.07+01.64
and AFGL 437 are located toward the opposite sides of the V-like structure, and
LBN 140.77$-$1.42 is spatially seen toward the linear part. Infrared-excess
sources are traced toward the entire Y-feature, suggesting star formation
activities. Infrared and sub-millimeter images show the presence of at least
two large-scale dust filaments extended toward the LBN sources. The Herschel
maps, which are available only toward the northern and central parts of the
Y-feature, display the presence of higher column density (> 2.4 X 10^{21}
cm^{-2}) of materials toward the filaments. Using the 12CO(1-0) line data, the
distribution of molecular gas at [-42.7, -34.4] km/s traces the cloud
associated with the Y-feature, and confirms the existence of filaments. The
large-scale filaments appear to be possibly spatially twisted. There is a hint
of an oscillatory-like velocity pattern along both the filaments, favouring
their proposed twisted nature. It is the first study showing the possible
twisting of filaments, which is more prominent in the northern and central
parts of the Y-feature. This possible twisting/coupling of the large-scale
filaments appears to be responsible for the observed star formation (including
known OB-stars). The proposed physical process and the energetics of OB-stars
together seem to explain the origin of the ionized Y-feature.
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