First robust detection of kpc-scale filamentary H I structures in the CGM/IGM around NGC 4631 with widths 0.5-3.3 kpc, lengths 6.1-49.8 kpc, and three kinematic classes (U-shaped, linear, wavy).
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3 Pith papers cite this work. Polarity classification is still indexing.
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astro-ph.GA 3years
2026 3verdicts
UNVERDICTED 3representative citing papers
3D wind-tunnel simulations in the χ~10^3 regime show clump-cocoon geometry sets SB_X/SB_Hα~3, with Hα fraction fixed by atomic physics and X-ray fraction set by residence time in the X-ray band that scales inversely with pressure.
TNG-Cluster simulations find that in galaxy cluster centers turbulence accounts for under half the total velocity dispersion (typically 50-75 km/s), is mostly subsonic, provides sub-percent pressure support, and is primarily driven by SMBH feedback.
citing papers explorer
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Highly filamentary H{\,\small I} gas in the circumgalactic medium and intragalactic medium around NGC 4631
First robust detection of kpc-scale filamentary H I structures in the CGM/IGM around NGC 4631 with widths 0.5-3.3 kpc, lengths 6.1-49.8 kpc, and three kinematic classes (U-shaped, linear, wavy).
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Clumps in a Cocoon: Geometry and Mixing Set the Universal X-ray to H$\alpha$ Surface Brightness Ratio
3D wind-tunnel simulations in the χ~10^3 regime show clump-cocoon geometry sets SB_X/SB_Hα~3, with Hα fraction fixed by atomic physics and X-ray fraction set by residence time in the X-ray band that scales inversely with pressure.
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Bulk vs. turbulent motions at the centres of galaxy clusters: AGN-driven turbulence according to TNG-Cluster
TNG-Cluster simulations find that in galaxy cluster centers turbulence accounts for under half the total velocity dispersion (typically 50-75 km/s), is mostly subsonic, provides sub-percent pressure support, and is primarily driven by SMBH feedback.