Formation of the Hub–Filament System G33.92+0.11: Local Interplay between Gravity, Velocity, and Magnetic Field

Wang, Jiawei; Koch, Patrick M.; Galván-Madrid, Roberto; Lai, Shih-Ping; Liu, Hauyu Baobab; Lin, Sheng-Jun; Pattle, Kate

doi:10.3847/1538-4357/abc74e

Cited by 34 publications

(33 citation statements)

References 89 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The interval between Sgr A * and SmR-3 is spanned by radial filaments in radio, Paschen-α, and X-ray wavebands (Figures 1(e), 2, and 10), interspersed with several near-IR-dark filaments of diminished X-ray emission that converge toward Sgr A * so are probably at the GC. The latter resemble dark "hub-filaments" that characterize star-forming molecular clouds elsewhere in the Galactic disk (Myers 2009) and generally align with the local gravity (e.g., Wang et al 2020) here dominated by Sgr A * within the much less massive CND (T18).…”

Section: At Ionized Nebula Smr-3supporting

confidence: 56%

Tracing the Milky Way's Vestigial Nuclear Jet

Cecil,

Wagner,

Bland-Hawthorn

et al. 2021

Preprint

View full text Add to dashboard Cite

MeerKAT radio continuum and XMM-Newton X-ray images have recently revealed a spectacular bipolar channel at the Galactic Center that spans several degrees (∼ 0.5 kpc). An intermittent jet likely formed this channel and is consistent with earlier evidence of a sustained, Seyfert-level outburst fueled by black-hole accretion onto Sgr A * several Myr ago. Therefore, to trace an intermittent jet that perhaps penetrated, deflected, and percolated along multiple paths through the interstellar medium, relevant interactions are identified and quantified in archival X-ray images, Hubble Space Telescope Paschen-α images and ALMA mm-wave spectra, and new SOAR telescope IR spectra. Hydrodynamical simulations are used to show how a currently weak jet can explain these structures and inflate the ROSAT/eROSITA X-ray and Fermi γ-ray bubbles that extend ±60 • from the Galactic plane. Thus, our Galactic outflow has features in common with energetic, jet-driven structures in the prototypical Seyfert galaxy NGC 1068.

show abstract

Section: At Ionized Nebula Smr-3supporting

confidence: 56%

Tracing the Milky Way's Vestigial Nuclear Jet

Cecil,

Wagner,

Bland-Hawthorn

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…This technique has been applied to FIR-sub-mm polarimetric observations of Galactic sources (i.e. Chapman et al 2011;Crutcher 2012;Girart et al 2013;Pattle et al 2017;Soam et al 2019;Chuss et al 2019;Redaelli et al 2019;Wang et al 2020;Guerra et al 2020;Michail et al 2021, Li et al in prep. ), as well as sub-mm polarimetric observations of external galaxies, like M51 (Houde et al 2013).…”

Section: The Angular Dispersion Functionmentioning

confidence: 99%

The strength and structure of the magnetic field in the galactic outflow of M82

Lopez-Rodriguez,

Guerra,

Asgari-Targhi

et al. 2021

Preprint

View full text Add to dashboard Cite

Galactic outflows driven by starbursts can modify the galactic magnetic fields and drive them away from the galactic planes. Here, we quantify how these fields may magnetize the intergalactic medium. We estimate the strength and structure of the fields in the starburst galaxy M82 using thermal polarized emission observations from SOFIA/HAWC+ and a potential field extrapolation. We modified the Davis-Chandrasekhar-Fermi method to account for the large-scale flow and the turbulent field. Results show that the observed magnetic fields arise from the combination of a large-scale ordered potential field associated with the outflow and a small-scale turbulent field associated with bow-shock-like features. Within the central 900 pc radius, the potential field accounts for 53 ± 4% of the observed turbulent magnetic energy with a median field strength of 305 ± 15 µG, while small-scale turbulent magnetic fields account for the remaining 40 ± 5% with a median field strength of 222 ± 19 µG. We estimate that the turbulent kinetic and turbulent magnetic energies are in close equipartition up to ∼ 2 kpc (measured), while the turbulent kinetic energy dominates at ∼ 7 kpc (extrapolated). We conclude that the fields are frozen into the ionized outflowing medium and driven away kinetically. This indicates that the magnetic field lines in the galactic wind of M82 are 'open,' providing a direct channel between the starburst core and the intergalactic medium. Our novel approach offers the tools needed to quantify the effects of outflows on galactic magnetic fields as well as their influence on the intergalactic medium and evolution of energetic particles.

show abstract

“…In addition to filament-filament collision, physical processes driven by gravitational instabilities, such as multi-scale gravitational collapse (Vázquez-Semadeni et al 2009;Gómez & Vázquez-Semadeni 2014;Gómez et al 2018) or layer fragmentation (Myers 2009;Van Loo et al 2014), are also proposed as a possible origin of HFSs. These theories are supported by the gravity-induced patterns found in magnetic field morphologies and the filament velocity structures (Myers 2009;Busquet et al 2013;Van Loo et al 2014;Wang et al 2019;Chen et al 2020;Wang et al 2020). However, the observed density and velocity structures only represent the current snapshot in time, and thus, it is difficult to constrain the forming environment of HFSs in the early evolutionary stage.…”

Section: Introductionmentioning

confidence: 99%

“…However, magnetic fields can be shaped by gravitational collapse and gravity-induced accretion flows (e.g., Crutcher 2012;Gómez et al 2018;Wang et al 2019). Generally, the detailed comparison between cloud/filament properties and magnetic field morphologies yields a useful tool to constrain the dominating physical process (e.g., Soler et al 2013;Koch et al 2012aKoch et al , 2013Koch et al , 2014bKoch et al , 2018Tahani et al 2018;Wang et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Formation of the SDC13 Hub-Filament System: A Cloud-Cloud Collision Imprinted on The Multiscale Magnetic Field

Wang,

Koch,

Tang

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

Hub-filament systems (HFSs) are potential sites of protocluster and massive star formation, and play a key role in mass accumulation. We report JCMT POL-2 850 µm polarization observations toward the massive HFS SDC13. We detect an organized magnetic field near the hub center with a cloudscale "U-shape" morphology following the western edge of the hub. Together with larger-scale APEX 13 CO and PLANCK polarization data, we find that SDC13 is located at the convergent point of three giant molecular clouds (GMCs) along a large-scale, partially spiral-like magnetic field. The smaller "U-shape" magnetic field is perpendicular to the large-scale magnetic field and the converging GMCs. We explain this as the result of a cloud-cloud collision. Within SDC13, we find that local gravity and velocity gradients point toward filament ridges and hub center. This suggests that gas can locally be pulled onto filaments and overall converges to the hub center. A virial analysis of the central hub shows that gravity dominates magnetic and kinematic energy. Combining large-and small-scale analyses, we propose that SDC13 is initially formed from a collision of clouds moving along the large-scale magnetic field. In the post-shock regions, after the initial turbulent energy has dissipated, gravity takes over and starts to drive the gas accretion along the filaments toward the hub center.

show abstract

Formation of the Hub–Filament System G33.92+0.11: Local Interplay between Gravity, Velocity, and Magnetic Field

Cited by 34 publications

References 89 publications

Tracing the Milky Way's Vestigial Nuclear Jet

Tracing the Milky Way's Vestigial Nuclear Jet

The strength and structure of the magnetic field in the galactic outflow of M82

Formation of the SDC13 Hub-Filament System: A Cloud-Cloud Collision Imprinted on The Multiscale Magnetic Field

Contact Info

Product

Resources

About