Filament rotation in the California L1482 cloud
  We analyze the gas mass distribution, the gas kinematics, and the young
stellar object (YSO) content of the California Molecular Cloud (CMC) L1482
filament. We derive a Gaia DR2 YSO distance of 511$^{+17}_{-16}$ pc. We derive
scale-free power-laws for the mean gas line-mass (M/L) profiles; we calculate
the gravitational potential and field profiles consistent with these. We
present IRAM 30 m C$^{18}$O (1-0) (and other tracers) position-velocity (PV)
diagrams that exhibit complex velocity twisting and turning structures. We find
a rotational profile in C$^{18}$O perpendicular to the southern filament
ridgeline. The profile is regular, confined ($r\lesssim0.4$ pc),
anti-symmetric, and to first order linear with a break at $r\sim0.25$ pc. The
timescales of the inner (outer) gradients are $\sim$0.7 (6.0) Myr. We show that
the centripetal force, compared to gravity, increases toward the break; when
the ratio of forces approaches unity, the profile turns over, just before
filament breakup is achieved. The timescales and relative roles of gravity to
rotation indicate that the structure is stable, long lived ($\sim$ a few times
6 Myr), and undergoing outside-in evolution. Moreover, this filament has
practically no star formation, a perpendicular Planck plane-of-the-sky (POS)
magnetic field morphology, and POS "zig-zag" morphology, which together with
the rotation profile lead to the suggestion that the 3D shape is a corkscrew
filament with a helical magnetic field. These results, combined with results in
Orion and G035.39-00.33, suggest evolution toward higher densities as rotating
filaments shed angular momentum. Thus, magnetic fields may be an essential
feature of high-mass (M $\sim10^5$ M$_{\odot}$) cloud filament evolution toward
cluster formation.
