A new Gaia-based catalogue identifies 57 kinematically coherent OB associations within 1 kpc of the Sun, twice as many as previously known, and finds most are expanding.
Overview of the Orion Complex
6 Pith papers cite this work, alongside 50 external citations. Polarity classification is still indexing.
6
Pith papers citing it
50
external citations · Pith
abstract
The Orion star formation complex is the nearest region of on-going star formation that continues to produce both low and high mass stars. Orion is discussed in the larger context of star formation in the Solar vicinity over the last 100 Myr. The Orion complex is located on the far side of the Gould's Belt system of clouds and young stars throughwhich our Solar systemis drifting. A review is given of the overall structure and properties of the Orion star forming complex, the best studied OB association. Over the last 12 Myr, Orion has given birth to at least ten thousand stars contained in a half dozen sub-groups and short-lived clusters. The Orion OB association has been the source of several massive, high-velocity run-away stars, including mu-Columbae and AE Aurigae. Some of Orion's most massive members died in supernova explosions that created the 300 pc diameter Orion / Eridanus super-bubble whose near wall may be as close as 180 pc. The combined effects of UV radiation, stellar winds, and supernovae have impacted surviving molecular clouds in Orion. The large Orion A, IC 2118 molecular clouds and dozens of smaller clouds strewn throughout the interior of the superbubble have cometary shapes pointing back towards the center of the Orion OB association. Most are forming stars in the compressed layers facing the bubble interior.
representative citing papers
TIME's SPACETIME pipeline yields calibrated spectral maps of OMC and G49.5 with <3% Bolocam flux agreement, demonstrating preliminary on-sky performance for future LIM surveys.
Gaia-derived parameters for 13 Orion clusters fed into N-body simulations reveal two regimes: seven with α_vir ≲ 7 retain bound cores for ≳170 Myr while six with α_vir ≳ 7 dissolve before 120 Myr.
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.
SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.
Reviews SKA techniques for reconstructing 3D magnetic field vectors in the ISM but presents no new data or derivations.
citing papers explorer
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A new Gaia census of OB associations within 1 kpc
A new Gaia-based catalogue identifies 57 kinematically coherent OB associations within 1 kpc of the Sun, twice as many as previously known, and finds most are expanding.
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TIME Commissioning Observations: II. On-sky Characterization and the 2D Map Data Processing Pipeline
TIME's SPACETIME pipeline yields calibrated spectral maps of OMC and G49.5 with <3% Bolocam flux agreement, demonstrating preliminary on-sky performance for future LIM surveys.
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Dynamical evolution and dissolution timescale of young stellar clusters in the Orion star-forming complex
Gaia-derived parameters for 13 Orion clusters fed into N-body simulations reveal two regimes: seven with α_vir ≲ 7 retain bound cores for ≳170 Myr while six with α_vir ≳ 7 dissolve before 120 Myr.
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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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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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3D Magnetic Field Vectors in Space: Bubbles, Clouds, and Filaments
Reviews SKA techniques for reconstructing 3D magnetic field vectors in the ISM but presents no new data or derivations.