Reveals a pristine scale-invariant 3D Kolmogorov turbulence cascade in the Polaris Flare with an analytical mapping showing the apparent transition arises from projection and density fractal dimension changes.
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From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt survey
12 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
We summarize the first results from the Gould Belt survey, obtained toward the Aquila Rift and Polaris Flare regions during the 'science demonstration phase' of Herschel. Our 70-500 micron images taken in parallel mode with the SPIRE and PACS cameras reveal a wealth of filamentary structure, as well as numerous dense cores embedded in the filaments. Between ~ 350 and 500 prestellar cores and ~ 45-60 Class 0 protostars can be identified in the Aquila field, while ~ unbound starless cores and no protostars are observed in the Polaris field. The prestellar core mass function (CMF) derived for the Aquila region bears a strong resemblance to the stellar initial mass function (IMF), already confirming the close connection between the CMF and the IMF with much better statistics than earlier studies. Comparing and contrasting our Herschel results in Aquila and Polaris, we propose an observationally-driven scenario for core formation according to which complex networks of long, thin filaments form first within molecular clouds, and then the densest filaments fragment into a number of prestellar cores via gravitational instability.
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Multi-scale observations of dense core G205.46-14.56-N2 show a quadruple protostellar system whose symmetry, outflows, and kinematics match simulations of rotational fragmentation, providing the first claimed evidence for this pathway in high-order multiples.
CARPP recovers seven core parameters from multi-band dust continuum via layered radiative transfer, achieving <20% average relative error under a stated noise-resolution criterion and classifying TMC-1C as near-critical Bonnor-Ebert and Ori2-2 as power-law collapsing.
PCA of 25 molecular lines across 1001 Orion B cores reveals that chemical diversity is driven by column density, the FUV-to-density ratio G0/n, and freeze-out signatures tied to mean density.
Linear decomposition of Planck dust maps using PMO CO and EBHIS HI surveys attributes 20-40% of dust to CO gas, negligible amounts to broad warm HI, and significant fractions to narrow cold HI and CO-dark molecular gas at boundaries.
Super-Serkowski UV polarization excesses are explained by enhanced RAT alignment under B-star EUV radiation (plus DG at the shortest wavelengths), while Serkowski curves are reproduced by RAT alone in cold neutral medium conditions.
Low-column-density filaments align parallel to magnetic fields while high-column-density wide filaments align perpendicular, with transition at roughly 0.8-8 x 10^21 cm^-2; projection effects analyzed statistically.
Observational study of MBM12 shows CO-to-H2 conversion factor near galactic average with density-dependent variations, high virial parameters decreasing at small scales, broken power-law mass-size relations indicating external pressure, and magnetic field orientation transition at N(H2) = 4.5e21 cm-
Oblique filament collisions lead to gravitational collapse of the compressed cloud when post-collision |gravitational energy| exceeds kinetic plus thermal plus magnetic energies, with lower angles and lower velocities favoring hub-filament formation.
3D modeling of L1506C with THEMIS 2 dust model shows evolved grains needed in densest regions, indicating early grain growth in prestellar phase.
SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.
HINSA observations show CRIR decreasing with H2 column density in both clouds, with IC 348 values an order of magnitude above NGC 1333, modeled as an order-of-magnitude difference in low-energy CR populations from local acceleration sources.
citing papers explorer
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Kolmogorov turbulence across multi-fractal gas in Polaris Flare
Reveals a pristine scale-invariant 3D Kolmogorov turbulence cascade in the Polaris Flare with an analytical mapping showing the apparent transition arises from projection and density fractal dimension changes.
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Formation of a Protostellar Multiple System via Rotational Fragmentation
Multi-scale observations of dense core G205.46-14.56-N2 show a quadruple protostellar system whose symmetry, outflows, and kinematics match simulations of rotational fragmentation, providing the first claimed evidence for this pathway in high-order multiples.
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CARPP: Parametric Radiative-Transfer Fitting of Molecular Cores from Dust Continuum Data
CARPP recovers seven core parameters from multi-band dust continuum via layered radiative transfer, achieving <20% average relative error under a stated noise-resolution criterion and classifying TMC-1C as near-critical Bonnor-Ebert and Ori2-2 as power-law collapsing.
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Chemical diversity of dense cores in Orion B: The role of the environment
PCA of 25 molecular lines across 1001 Orion B cores reveals that chemical diversity is driven by column density, the FUV-to-density ratio G0/n, and freeze-out signatures tied to mean density.
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PMO Polaris CO survey. II. Where is the dust?
Linear decomposition of Planck dust maps using PMO CO and EBHIS HI surveys attributes 20-40% of dust to CO gas, negligible amounts to broad warm HI, and significant fractions to narrow cold HI and CO-dark molecular gas at boundaries.
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Grain Alignment and Dust Evolution Physics with Polarisation (GRADE-POL). II. On the physical basis of Serkowski and super-Serkowski polarisation spectra
Super-Serkowski UV polarization excesses are explained by enhanced RAT alignment under B-star EUV radiation (plus DG at the shortest wavelengths), while Serkowski curves are reproduced by RAT alone in cold neutral medium conditions.
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Statistical analysis of the relative orientations between filaments and magnetic fields using Herschel and Planck data in star-forming regions
Low-column-density filaments align parallel to magnetic fields while high-column-density wide filaments align perpendicular, with transition at roughly 0.8-8 x 10^21 cm^-2; projection effects analyzed statistically.
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B-Fields and Star Formation across Scales with TRAO (B-FROST): CO Abundances, Dynamics and Relative Orientations in the Translucent High Latitude Cloud MBM12
Observational study of MBM12 shows CO-to-H2 conversion factor near galactic average with density-dependent variations, high virial parameters decreasing at small scales, broken power-law mass-size relations indicating external pressure, and magnetic field orientation transition at N(H2) = 4.5e21 cm-
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Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions
Oblique filament collisions lead to gravitational collapse of the compressed cloud when post-collision |gravitational energy| exceeds kinetic plus thermal plus magnetic energies, with lower angles and lower velocities favoring hub-filament formation.
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Tracing grain growth in the forming prestellar core L1506C with 3D modeling of Herschel, IRAM, and CFHT observations
3D modeling of L1506C with THEMIS 2 dust model shows evolved grains needed in densest regions, indicating early grain growth in prestellar phase.
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Early phases of star formation with SKAO: synchrotron emission from dense starless cores in molecular clouds
SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.
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A HINSA view of cosmic-ray ionization in IC 348 and NGC 1333: evidence for a strong low-energy cosmic-ray disparity
HINSA observations show CRIR decreasing with H2 column density in both clouds, with IC 348 values an order of magnitude above NGC 1333, modeled as an order-of-magnitude difference in low-energy CR populations from local acceleration sources.