Independent Core Rotation in Massive Filaments in Orion. (arXiv:2004.14643v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Xu_X/0/1/0/all/0/1">Xuefang Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_D/0/1/0/all/0/1">Di Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_Y/0/1/0/all/0/1">Y.Sophia Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fuller_G/0/1/0/all/0/1">Gary A. Fuller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yue_N/0/1/0/all/0/1">Nannan Yue</a>
We present high-angular-resolution ALMA (Atacama Large Millimeter Array)
images of N$_{2}$H$^{+}$ (1–0) that has been combined with those from the
Nobeyama telescope toward OMC-2 and OMC-3 filamentary regions. The filaments
(with typical widths of $sim$ 0.1 pc) and dense cores are resolved. The
measured 2D velocity gradients of cores are between 1.3 and 16.7
km,s$^{-1}$,pc$^{-1}$, corresponding to a specific angular momentum ($J/M$)
between 0.0012 and 0.016 pc,km,s$^{-1}$. With respect to the core size $R$,
the specific angular momentum follows a power law $J/M propto
R^{1.52~pm~0.14}$. The ratio ($beta$) between the rotational energy and
gravitational energy ranges from 0.00041 to 0.094, indicating insignificant
support from rotation against gravitational collapse. We further focus on the
alignment between the cores’ rotational axes, which is defined to be
perpendicular to the direction of the velocity gradient ($theta_{G}$), and the
direction of elongation of filaments ($theta_{f}$) in this massive
star-forming region. The distribution of the angle between $theta_{f}$ and
$theta_{G}$ was f ound to be random, i.e. the cores’ rotational axes have no
discernible correlation with the elongation of their hosting filament. This
implies that, in terms of angular momentum, the cores have evolved to be
dynamically independent from their natal filaments.
We present high-angular-resolution ALMA (Atacama Large Millimeter Array)
images of N$_{2}$H$^{+}$ (1–0) that has been combined with those from the
Nobeyama telescope toward OMC-2 and OMC-3 filamentary regions. The filaments
(with typical widths of $sim$ 0.1 pc) and dense cores are resolved. The
measured 2D velocity gradients of cores are between 1.3 and 16.7
km,s$^{-1}$,pc$^{-1}$, corresponding to a specific angular momentum ($J/M$)
between 0.0012 and 0.016 pc,km,s$^{-1}$. With respect to the core size $R$,
the specific angular momentum follows a power law $J/M propto
R^{1.52~pm~0.14}$. The ratio ($beta$) between the rotational energy and
gravitational energy ranges from 0.00041 to 0.094, indicating insignificant
support from rotation against gravitational collapse. We further focus on the
alignment between the cores’ rotational axes, which is defined to be
perpendicular to the direction of the velocity gradient ($theta_{G}$), and the
direction of elongation of filaments ($theta_{f}$) in this massive
star-forming region. The distribution of the angle between $theta_{f}$ and
$theta_{G}$ was f ound to be random, i.e. the cores’ rotational axes have no
discernible correlation with the elongation of their hosting filament. This
implies that, in terms of angular momentum, the cores have evolved to be
dynamically independent from their natal filaments.
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