Trapezium Cluster

Trapezium Cluster
Public domain · source
Name	Trapezium Cluster
Epoch	J2000
Constellation	Orion
Distance	1344 ly
Notes	Open cluster in the Orion Nebula

Contents

Trapezium Cluster The Trapezium Cluster is a compact open cluster at the heart of the Orion Nebula that serves as a laboratory for studies of stellar formation, early stellar evolution, and cluster dynamics, and it influences the surrounding Orion Molecular Cloud Complex, Great Orion Nebula, M42, and nearby star-forming regions such as Belt of Orion. The cluster's bright members ionize the nebula and are central to investigations by observatories including the Hubble Space Telescope, the Chandra X-ray Observatory, the Atacama Large Millimeter/submillimeter Array, and the Very Large Telescope. Studies of the cluster connect to research institutions like the Harvard–Smithsonian Center for Astrophysics, the Max Planck Institute for Astronomy, and the European Southern Observatory.

Overview

The compact core contains several O- and B-type stars discovered during surveys by observers associated with William Herschel, John Herschel, and later cataloged by the Royal Astronomical Society and the Harvard College Observatory, while modern imaging by the Palomar Observatory and the Keck Observatory resolved proplyds and multiplicity. The cluster lies within the Orion A filament of the Orion Molecular Cloud Complex, near massive regions studied by teams from NASA, the European Space Agency, and the National Research Council (Canada), and it influences the ionization front observed in maps from the Spitzer Space Telescope and the James Webb Space Telescope. The immediate environment connects to features named by early surveys such as the Messier catalogue and the New General Catalogue that chart bright nebular objects in Orion (constellation).

The brightest core stars are massive O-type and B-type systems whose spectral classification links to standards used by researchers at the Mount Wilson Observatory, the Cerro Tololo Inter-American Observatory, and the University of California, Berkeley astronomy department. Multiplicity surveys by teams from the California Institute of Technology, the University of Cambridge, and the University of Toronto have revealed hierarchical systems analogous to those in clusters studied by the Sloan Digital Sky Survey and modeled in numerical work at the Princeton University astrophysics group and the Max Planck Institute for Astrophysics. X-ray studies by the Chandra X-ray Observatory and infrared imaging by the Spitzer Space Telescope and the Two Micron All-Sky Survey show pre-main-sequence stars with excess emission similar to objects cataloged by the Infrared Astronomical Satellite and the Wide-field Infrared Survey Explorer. Mass estimates employ evolutionary tracks developed by groups including researchers at the Geneva Observatory, the University of Bonn, and the University of Arizona, while extinction and reddening measurements reference standards from the Cerro Tololo Inter-American Observatory and the European Southern Observatory.

Models of cluster formation incorporate gravitational collapse in filaments first characterized in surveys by the James Clerk Maxwell Telescope and the Submillimeter Array, and numerical simulations performed by teams at the Harvard-Smithsonian Center for Astrophysics, the Max Planck Institute for Radio Astronomy, and the California Institute of Technology. Feedback processes from massive stars are compared to cases studied in the Carina Nebula and the Pillars of Creation region in the Eagle Nebula, with radiation-hydrodynamics modeled using codes developed at the Princeton University, the University of Oxford, and the École Normale Supérieure. Dynamical evolution, mass segregation, and possible ejection of runaway stars have been analyzed in the context of results from the Gaia mission, the Hipparcos satellite, and long-term radial-velocity monitoring programs at the Anglo-Australian Observatory and the Observatoire de Paris.

Intense ultraviolet radiation and stellar winds from the cluster’s massive members shape ionization fronts, photoevaporative flows, and protoplanetary disk erosion observable in imagery from the Hubble Space Telescope, the Atacama Large Millimeter/submillimeter Array, and the Subaru Telescope, and are studied alongside similar phenomena in the Rosette Nebula and the Horsehead Nebula. The cluster’s influence on the Orion Bar photodissociation region and associated molecular chemistry ties into spectroscopic surveys carried out by teams at the Institut d'Astrophysique de Paris, the National Radio Astronomy Observatory, and the Max Planck Institute for Extraterrestrial Physics, while cosmic-ray and magnetic-field interactions are probed by instruments from the Fermi Gamma-ray Space Telescope and ground arrays such as the High Energy Stereoscopic System.

Early optical observations by Galileo Galilei and cataloging by Charles Messier through the Messier catalogue led into spectroscopic work at the Dunlap Observatory and photometric campaigns at the Royal Observatory, Greenwich, and later high-resolution imaging with the Hubble Space Telescope revealed proplyds that galvanized studies at the Space Telescope Science Institute, the European Southern Observatory, and the National Optical Astronomy Observatory. X-ray surveys by the Chandra X-ray Observatory and infrared programs with the Spitzer Space Telescope and the James Webb Space Telescope provided deep censuses compared with catalogs from the Two Micron All-Sky Survey and the Sloan Digital Sky Survey. Landmark theoretical and observational reviews have been produced by researchers affiliated with the Harvard College Observatory, the Max Planck Society, and the Royal Astronomical Society, and continue to inform campaigns using facilities such as the Very Large Array, the Keck Observatory, and the Gemini Observatory.