210 research outputs found
An Imprint of Molecular Cloud Magnetization in the Morphology of the Dust Polarized Emission
We describe a morphological imprint of magnetization found when considering
the relative orientation of the magnetic field direction with respect to the
density structures in simulated turbulent molecular clouds. This imprint was
found using the Histogram of Relative Orientations (HRO): a new technique that
utilizes the gradient to characterize the directionality of density and column
density structures on multiple scales. We present results of the HRO analysis
in three models of molecular clouds in which the initial magnetic field
strength is varied, but an identical initial turbulent velocity field is
introduced, which subsequently decays. The HRO analysis was applied to the
simulated data cubes and mock-observations of the simulations produced by
integrating the data cube along particular lines of sight. In the 3D analysis
we describe the relative orientation of the magnetic field with
respect to the density structures, showing that: 1.The magnetic field shows a
preferential orientation parallel to most of the density structures in the
three simulated cubes. 2.The relative orientation changes from parallel to
perpendicular in regions with density over a critical density in the
highest magnetization case. 3.The change of relative orientation is largest for
the highest magnetization and decreases in lower magnetization cases. This
change in the relative orientation is also present in the projected maps. In
conjunction with simulations HROs can be used to establish a link between the
observed morphology in polarization maps and the physics included in
simulations of molecular clouds.Comment: (16 pages, 11 figures, submitted to ApJ 05MAR2013, accepted
07JUL2013
Tracing H2 column density with atomic carbon (CI) and CO isotopologues
We present first results of neutral carbon ([CI], 3P1 - 3P0 at 492 GHz) and
carbon monoxide (13CO, J = 1 - 0) mapping in the Vela Molecular Ridge cloud C
(VMR-C) and G333 giant molecular cloud complexes with the NANTEN2 and Mopra
telescopes. For the four regions mapped in this work, we find that [CI] has
very similar spectral emission profiles to 13CO, with comparable line widths.
We find that [CI] has opacity of 0.1 - 1.3 across the mapped region while the
[CI]/13CO peak brightness temperature ratio is between 0.2 to 0.8. The [CI]
column density is an order of magnitude lower than that of 13CO. The H2 column
density derived from [CI] is comparable to values obtained from 12CO. Our maps
show CI is preferentially detected in gas with low temperatures (below 20 K),
which possibly explains the comparable H2 column density calculated from both
tracers (both CI and 12CO underestimate column density), as a significant
amount of the CI in the warmer gas is likely in the higher energy state
transition ([CI], 3P2 - 3P1 at 810 GHz), and thus it is likely that
observations of both the above [CI] transitions are needed in order to recover
the total H2 column density.Comment: accepted for publication in ApJ Letter
SOFIA and ALMA Investigate Magnetic Fields and Gas Structures in Massive Star Formation: The Case of the Masquerading Monster in BYF 73
We present SOFIA+ALMA continuum and spectral-line polarisation data on the
massive molecular cloud BYF 73, revealing important details about the magnetic
field morphology, gas structures, and energetics in this unusual massive star
formation laboratory. The 154m HAWC+ polarisation map finds a highly
organised magnetic field in the densest, inner 0.550.40 pc portion of
the cloud, compared to an unremarkable morphology in the cloud's outer layers.
The 3mm continuum ALMA polarisation data reveal several more structures in the
inner domain, including a pc-long, 500 M "Streamer" around the
central massive protostellar object MIR 2, with magnetic fields mostly parallel
to the east-west Streamer but oriented north-south across MIR 2. The magnetic
field orientation changes from mostly parallel to the column density structures
to mostly perpendicular, at thresholds = 6.610
m, = 2.510 m, and =
427 nT. ALMA also mapped Goldreich-Kylafis polarisation in CO
across the cloud, which traces in both total intensity and polarised flux, a
powerful bipolar outflow from MIR 2 that interacts strongly with the Streamer.
The magnetic field is also strongly aligned along the outflow direction;
energetically, it may dominate the outflow near MIR 2, comprising rare evidence
for a magnetocentrifugal origin to such outflows. A portion of the Streamer may
be in Keplerian rotation around MIR 2, implying a gravitating mass 135050
M for the protostar+disk+envelope; alternatively, these kinematics
can be explained by gas in free fall towards a 95035 M object.
The high accretion rate onto MIR 2 apparently occurs through the Streamer/disk,
and could account for 33% of MIR 2's total luminosity via gravitational
energy release.Comment: 33 pages, 32 figures, accepted by ApJ. Line-Integral Convolution
(LIC) images and movie versions of Figures 3b, 7, and 29 are available at
https://gemelli.spacescience.org/~pbarnes/research/champ/papers
Circulation in the vicinity of Mackenzie Canyon from a year-long mooring array
© The Author(s), 2020. This article is distributed under the terms of the Creative Commons Attribution License. The definitive version was published in Lin, P., Pickart, R. S., Fissel, D., Ross, E., Kasper, J., Bahr, F., Torres, D. J., O'Brien, J., Borg, K., Melling, H., & Wiese, F. K. Circulation in the vicinity of Mackenzie Canyon from a year-long mooring array. Progress in Oceanography, 187, (2020): 102396, doi:10.1016/j.pocean.2020.102396.Data from a five-mooring array extending from the inner shelf to the continental slope in the vicinity of Mackenzie Canyon, Beaufort Sea are analyzed to elucidate the components of the boundary current system and their variability. The array, part of the Marine Arctic Ecosystem Study (MARES), was deployed from October 2016 to September 2017. Four distinct currents were identified: an eastward-directed flow adjacent to the coast; a westward-flowing, surface-intensified current centered on the outer-shelf; a bottom-intensified shelfbreak jet flowing to the east; and a recirculation at the base of the continental slope within the canyon. The shelf current transports −0.120.03 Sv in the mean and is primarily wind-driven. The response is modulated by the presence of ice, with little-to-no signal during periods of nearly-immobile ice cover and maximum response when there is partial ice cover. The shelfbreak jet transports 0.030.02 Sv in the mean, compared to 0.080.02 Sv measured upstream in the Alaskan Beaufort Sea over the same time period. The loss of transport is consistent with a previous energetics analysis and the lack of Pacific-origin summer water downstream. The recirculation in the canyon appears to be the result of local dynamics whereby a portion of the westward-flowing southern limb of the Beaufort Gyre is diverted up the canyon across isobaths. This interpretation is supported by the fact that the low-frequency variability of the recirculation is correlated with the wind-stress curl in the Canada Basin, which drives the Beaufort gyre.The authors are indebted to Fisheries and Oceans Canada for building the logistics for MARES into the at-sea missions of the Integrated Beaufort Observatory. We are grateful to the captain and crew of the CCGS Sir Wilfred Laurier for ably deploying and recovering the MARES array. Marshall Swartz assisted with the cruise preparation logistics. We thank the two anonymous reviewers for their input which helped improve the paper. This project was funded by the US Bureau of Ocean Energy Management (BOEM), on behalf of the National Ocean Partnership Program. The Canadian contribution was supported by the Environmental Studies Research Fund (ESRF Project 2014-02N). MARES publication 003
The balloon-borne large-aperture submillimeter telescope for polarimetry: BLAST-Pol
The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry
(BLAST-Pol) is a suborbital mapping experiment designed to study the role
played by magnetic fields in the star formation process. BLAST-Pol is the
reconstructed BLAST telescope, with the addition of linear polarization
capability. Using a 1.8 m Cassegrain telescope, BLAST-Pol images the sky onto a
focal plane that consists of 280 bolometric detectors in three arrays,
observing simultaneously at 250, 350, and 500 um. The diffraction-limited
optical system provides a resolution of 30'' at 250 um. The polarimeter
consists of photolithographic polarizing grids mounted in front of each
bolometer/detector array. A rotating 4 K achromatic half-wave plate provides
additional polarization modulation. With its unprecedented mapping speed and
resolution, BLAST-Pol will produce three-color polarization maps for a large
number of molecular clouds. The instrument provides a much needed bridge in
spatial coverage between larger-scale, coarse resolution surveys and narrow
field of view, and high resolution observations of substructure within
molecular cloud cores. The first science flight will be from McMurdo Station,
Antarctica in December 2010.Comment: 14 pages, 9 figures Submitted to SPIE Astronomical Telescopes and
Instrumentation Conference 201
- …