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| Scorpius–Centaurus Association | |
|---|---|
| Name | Scorpius–Centaurus Association |
| Alias | Sco–Cen |
| Constellation | Scorpius, Centaurus |
| Distance | ~100–200 pc |
| Age | ~10–17 Myr |
| Members | ~1000+ |
| Notable members | Alpha Centauri, Beta Centauri, Antares, Fomalhaut? |
Scorpius–Centaurus Association is the nearest OB stellar association to the Solar System and a major young stellar grouping in the southern sky, located across the constellations Scorpius and Centaurus. It links to many observational programs and institutions such as Hipparcos, Gaia, Hubble Space Telescope, Chandra X-ray Observatory, Spitzer Space Telescope and surveys like 2MASS, WISE, ROSAT, ALMA, and VLT that have characterized its membership, kinematics, ages, and circumstellar material. The association is central to studies by researchers affiliated with ESO, Caltech, MIT, Harvard–Smithsonian, Max Planck Institute for Astronomy, and programs including Sloan Digital Sky Survey, Gaia-ESO Survey, and individual projects led by astronomers at University of Chicago, University of California, Berkeley, University of Arizona, University of Toronto, and Australian National University.
The association spans a sky region studied by teams using facilities such as Anglo-Australian Telescope, Keck Observatory, Gemini Observatory, Subaru Telescope, and Magellan and is often separated into coherent groups in analyses by de Zeeuw et al., Pecaut, Mamajek, Preibisch, Sartori, and collaborations at University of Michigan and Pennsylvania State University. It connects to larger structures like the Local Bubble, Gould Belt, and nearby associations including Tucana–Horologium Association, Beta Pictoris Moving Group, Columba Association, and Carina–Near Moving Group. Major facilities such as European Space Agency and NASA missions have driven mapping efforts, while ground programs at Carnegie Observatories and AAO provided spectroscopic follow-up.
The association is classically divided into three principal subgroups identified in work by Blaauw, de Zeeuw, Preibisch and Mamajek: Upper Scorpius, Upper Centaurus–Lupus, and Lower Centaurus–Crux, with membership catalogs expanded by Rizzuto, Kraus, Song, Pecaut, Luhman, Slesnick, and teams at Arizona State University and University of Colorado Boulder. Prominent individual stars historically associated through kinematic or photometric criteria include members of stellar systems studied at Cerro Tololo Inter-American Observatory and Siding Spring Observatory and target lists compiled by ESO Science Archive Facility and Mikulski Archive for Space Telescopes. Membership assessments have used proper motions from Hipparcos and Gaia combined with radial velocities from instruments like HARPS, UVES, HIRES, and spectrographs on Magellan.
Star formation in the association has been analyzed in papers by Preibisch, Mamajek, Soderblom, Palla, Stahler, and others using isochrones from model grids by Siess, Baraffe, Bressan, Dotter and PARSEC (stellar). Ages vary between subgroups with Upper Scorpius commonly cited at ~10 Myr and Upper Centaurus–Lupus and Lower Centaurus–Crux at ~15–17 Myr in studies from Mamajek & Feigelson, Pecaut & Mamajek, and analyses using Gaia DR2 and Gaia EDR3 by Cantat-Gaudin, Kounkel, and Zari. Star formation episodes have been linked to supernovae and feedback scenarios discussed by Bally, Elmegreen, Hartmann, and investigations into triggered star formation near the Lupus and Chamaeleon clouds.
Kinematic structure has been mapped with astrometry from Hipparcos and Gaia and radial-velocity programs by teams at ESO, Keck Observatory, and McDonald Observatory, building on theoretical frameworks by Blaauw, Ambartsumian, Lynden-Bell, and dynamical analyses employing N-body codes developed by groups at Cambridge University, Princeton University, Rutgers University, and Max Planck Institute for Astrophysics. Studies by de Zeeuw, Rizzuto, Kraus, Mamajek, and Dahm have characterized expansion signatures, substructure, and velocity dispersions that inform constraints on dispersal timescales, tidal influences from the Galactic disk and passages near the Local Standard of Rest, and perturbations from nearby massive stars such as those cataloged in Bright Star Catalogue.
The association contains O-type, B-type, A-type, F-type, G-type, K-type, and M-type stars cataloged in works by Pecaut, Luhman, Soderblom, Preibisch, and Rizzuto, with spectral classifications anchored to standards maintained by Mount Wilson Observatory and spectral libraries from ESO. High-mass stars and evolved objects like Antares and bright B-stars have been subjects in studies by Dupree and Hillenbrand, while low-mass members and brown dwarfs have been identified by Lodieu, Kirkpatrick, and surveys including UKIDSS and VISTA. X-ray activity, lithium abundances, rotation rates, and accretion indicators have been measured with Chandra, XMM-Newton, Kepler, and spectrographs used by teams at Harvard–Smithsonian, MIT Kavli Institute, and Institute for Astronomy, University of Hawaii.
Debris disks and protoplanetary systems in the association have been imaged and characterized by Spitzer, Herschel, ALMA, VLA, and adaptive optics systems on Keck, VLT, and Gemini South, with interpretations by researchers at Caltech, University of Arizona, University of California, Los Angeles, and Jet Propulsion Laboratory. Notable disk-hosting stars linked to exoplanet and disk studies include targets overlapping catalogs from NASA Exoplanet Archive, Exoplanet.eu, and surveys led by Marois, Kalas, Lagrange, and Kasper. Direct imaging campaigns and radial-velocity programs have searched for companions using instruments like GPI, SPHERE, NACO, and CRIRES; circumstellar debris has been modeled with tools and codes from groups at Geneva Observatory, Leiden Observatory, and Max Planck Institute for Astronomy.
Identification and early studies were advanced by astronomers including Blaauw, de Zeeuw, Crawford, Garrison, and later by surveys such as Hipparcos and ROSAT that provided astrometric and X-ray membership indicators, followed by deep photometric and spectroscopic campaigns by 2MASS, WISE, Spitzer, and ground-based programs from CTIO, AAO, and ESO observatories. Contemporary refinements using Gaia DR2, Gaia EDR3, and ongoing Gaia data releases, combined with radial-velocity projects at ESO and Keck, have led to large catalogs and papers by collaborative teams across institutions like University of Cambridge, University of Edinburgh, University of Melbourne, National Astronomical Observatory of Japan, and Shanghai Astronomical Observatory.
Category:Stellar associations