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| Grand-design spiral galaxies | |
|---|---|
| Name | Grand-design spiral galaxy |
| Type | SA(s)b–SB(s)b |
| Epoch | J2000 |
Grand-design spiral galaxies are galaxies characterized by prominent, well-defined spiral arms that extend clearly around their disks. They are exemplars in studies of Andromeda Galaxy, Messier 51, and other nearby systems and serve as laboratories for testing theories developed by researchers associated with Institute for Advanced Study, Max Planck Society, and observatories such as Palomar Observatory and Hubble Space Telescope. Their striking morphology has been central to projects at institutions like Harvard–Smithsonian Center for Astrophysics and collaborations involving European Southern Observatory and National Radio Astronomy Observatory.
Grand-design spirals are classified within traditional schemes developed at Mount Wilson Observatory and refined by systems used at Carnegie Institution for Science and Royal Observatory, Greenwich. In the Hubble sequence and extensions implemented by Edwin Hubble and later by Allan Sandage, these systems correspond to the well-ordered SA and SB classes with two dominant arms, often catalogued in compilations such as the New General Catalogue and studies from Sloan Digital Sky Survey. Classification work by teams at European Space Agency and National Aeronautics and Space Administration ties visual arm prominence to metrics used by Spitzer Space Telescope surveys.
The morphology of these galaxies includes prominent stellar arms, a central bulge, and sometimes a bar, features explored in detail in observations from Very Large Telescope, Keck Observatory, and Gemini Observatory. Arms show contrast in stellar density traced by surveys carried out by Two Micron All Sky Survey and GALEX and are observed in molecular gas by arrays such as Atacama Large Millimeter/submillimeter Array and Very Large Array. Spiral pitch angle measurements used in papers from Max Planck Institute for Astronomy and studies referencing the Tully–Fisher relation relate arm geometry to disk rotation and mass distribution studied in contexts like Vera C. Rubin Observatory planning.
Theoretical frameworks credited to researchers at Princeton University, Cambridge University, and University of California, Berkeley include density wave theory formulated by scholars affiliated with University of Colorado Boulder and mechanisms involving tidal interactions studied in work on Messier 51 by groups at Yale University and Columbia University. Interactions with companions catalogued in surveys by Anglo-Australian Observatory and dynamical analyses from Rutgers University explain arm triggering in cases such as M51 interacting with NGC 5195. Alternative explanations developed in the literature from California Institute of Technology and University of Chicago invoke swing amplification and modal theories applied in simulations by teams at Jet Propulsion Laboratory and Lawrence Berkeley National Laboratory.
Star formation along arms is documented in studies by Carnegie Mellon University and projects using instruments on Chandra X-ray Observatory and Spitzer Space Telescope, revealing correlations with molecular clouds identified by Institute of Astrophysics of Andalusia and surveys like COBE. Observational programs led by University of Toronto and University of Cambridge connect H II region distributions to feedback processes discussed in literature from Imperial College London and University of Edinburgh. Dust lanes and cold gas reservoirs mapped by Herschel Space Observatory and Planck (spacecraft) are central to interpreting the interstellar medium properties in arms.
Well-studied examples include Messier 51, NGC 628, NGC 1566, M101, and Andromeda Galaxy, each observed by facilities such as Hubble Space Telescope, Spitzer Space Telescope, and Atacama Large Millimeter/submillimeter Array. Surveys by Sloan Digital Sky Survey and citizen science projects at Zooniverse have expanded samples used in comparative work by teams at University of Oxford and University of Wisconsin–Madison. Multiwavelength programs from Space Telescope Science Institute and analyses connected to catalogs like Third Reference Catalogue of Bright Galaxies document rotation curves, arm contrast, and bar coupling.
Grand-design spirals influence secular evolution in pathways analyzed in theoretical work from Princeton University and observational programs at University of Pennsylvania. Bars and spiral arms redistribute angular momentum in manners discussed in studies associated with Massachusetts Institute of Technology and University of Michigan, driving central star formation and pseudobulge growth noted in papers linked to Max Planck Institute for Astrophysics. Environmental effects from group and cluster contexts in catalogs produced by Two Micron All Sky Survey and Sloan Digital Sky Survey affect longevity of grand-design structure as examined by researchers at Cavendish Laboratory and University of Leiden.
High-resolution simulations produced by teams at Los Alamos National Laboratory, National Center for Supercomputing Applications, and Oak Ridge National Laboratory implement physics used in models from University of Washington and University of Illinois Urbana-Champaign. Codes such as those developed in collaborations involving Princeton Plasma Physics Laboratory and projects at Argonne National Laboratory reproduce spiral modes, tidal triggering, and gas feedback consistent with analytic work by scholars connected to University of Cambridge and Columbia University. Comparative studies leveraging computing resources at Fermi National Accelerator Laboratory and supercomputers commissioned by National Science Foundation provide constraints tested against observations from Hubble Space Telescope and Atacama Large Millimeter/submillimeter Array.
Category:Spiral galaxies