This article was accepted into the corpus but its outbound wikilinks were never NER-processed — typical at the deepest BFS hop or when the run's entity cap was reached. No expansion funnel to show.
| W43 complex | |
|---|---|
| Name | W43 complex |
| Type | Star-forming complex |
| Constellation | Scutum |
| Epoch | J2000 |
| Distance | ~5.5 kpc |
| Coordinates | 18h47m, −01°45′ |
| Other names | W43 Main, W43 South, G30.8−0.0 |
W43 complex is a massive, dense star-forming complex in the inner Milky Way noted for prolific high-mass star formation and rich molecular environment. The region lies near the intersection of the Galactic bar and the Scutum–Centaurus arm, hosting young stellar clusters, H II regions, and infrared dark clouds. W43 has been a target of multiwavelength campaigns involving radio, infrared, submillimeter, and millimeter facilities.
W43 is associated with prominent H II regions, infrared sources, and maser emission identified in surveys by IRAS, Spitzer Space Telescope, Herschel Space Observatory, and the Very Large Array. The complex includes both an active cluster of OB stars and compact objects traced by methanol masers and water masers; it is often compared to other massive star-forming sites such as W49A, W51, Orion Nebula and Carina Nebula. W43 serves as a local analog for extragalactic starburst regions observed in galaxies like M82 and NGC 253.
W43 contains multiple subregions commonly labelled in the literature, including dense clumps and compact H II regions cataloged in surveys by the ATLASGAL and BGPS teams. The complex comprises infrared clusters similar to those cataloged by 2MASS and UKIDSS, dense filamentary networks reminiscent of structures in Aquila Rift and Taurus Molecular Cloud, and massive cores analogous to protoclusters in G0.253+0.016. Embedded OB associations in W43 show spectral features comparable to members of Cygnus X and NGC 3603. The ionized gas and photodissociation regions have morphologies paralleling those in RCW 49 and NGC 6357.
W43 hosts prolific high-mass star formation including O-type and early B-type stars identified through radio recombination lines and infrared spectroscopy from facilities such as VLT and Keck Observatory. Young stellar objects and massive protostars in W43 display maser activity similar to sources studied with the European VLBI Network and Very Long Baseline Array. The initial mass function and cluster mass in W43 are compared with results from Orion Nebula Cluster and Westerlund 2, and the complex is considered a candidate for forming massive bound clusters like Arches Cluster and Quintuplet Cluster.
Molecular inventories in W43 include abundant CO isotopologues mapped by the FCRAO and Nobeyama Radio Observatory, dense gas tracers such as HCN, HCO+, and N2H+ observed with IRAM 30m and ALMA, and complex organic molecules similar to detections in Sgr B2. Kinematic studies reveal large velocity dispersions and converging flows consistent with cloud collisions invoked in models for regions like W51 and DR21. Filamentary inflow and hub–filament systems in W43 are analogous to structures cataloged by Herschel Gould Belt Survey and interpreted in the context of global collapse scenarios studied in Perseus molecular cloud.
W43 is located in the inner Galaxy near the tangent of the Scutum–Centaurus Arm and close to the bar end, with distance estimates around 5–6 kiloparsecs derived from kinematic measurements and maser parallax studies by groups using the VLBA and VERA. Its Galactocentric position places it near other massive complexes such as G30.79−0.05 and the Scutum arm complexes studied alongside W44 and W47 in large-scale surveys like COBE and GLIMPSE.
W43 has been observed across the spectrum: infrared mapping by Spitzer Space Telescope and WISE, far-infrared and submillimeter imaging by Herschel Space Observatory and APEX under programs including Hi-GAL and ATLASGAL, radio continuum and maser surveys by the VLA, Effelsberg Radio Telescope, and the Methanol Multibeam Survey. High-resolution interferometry with ALMA and the SMA has probed cores and outflows, while CO and dense-gas kinematics have been mapped by projects using the FCRAO and Nobeyama Radio Observatory.
Theoretical interpretations of W43 invoke models such as turbulent fragmentation, global hierarchical collapse, and cloud–cloud collision scenarios explored in numerical work by authors using magnetohydrodynamic codes comparable to studies applied to Giant Molecular Clouds in M51 and NGC 6946. W43 is significant as a nearby laboratory for massive cluster formation processes relevant to starburst regions in galaxies like M83 and M51, and for testing feedback models that include ionizing radiation, stellar winds, and supernovae analogous to feedback in 30 Doradus.
Category:Star-forming regions Category:Milky Way