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| Sombrero Galaxy | |
|---|---|
| Name | Sombrero Galaxy |
| Type | SA(s)a |
| Epoch | J2000 |
| Constellation | Virgo |
| Distance | 9.55 Mpc |
| Redshift | 0.0034 |
| Apparent magnitude | 8.0 |
| Size | 12′ × 6′ |
| Names | M104, NGC 4594 |
Sombrero Galaxy The Sombrero Galaxy is a prominent nearby spiral galaxy notable for its large central bulge and dust lane, frequently imaged by Hubble Space Telescope, Very Large Telescope, Spitzer Space Telescope, Chandra X-ray Observatory, and Arecibo Observatory. It is cataloged as Messier 104 and NGC 4594 and lies in the direction of the Virgo constellation near the Virgo Cluster. The galaxy is an important target for studies by researchers from institutions such as the European Southern Observatory, National Aeronautics and Space Administration, Space Telescope Science Institute, and Harvard–Smithsonian Center for Astrophysics.
The galaxy appears as a nearly edge-on disk with a striking dust lane and luminous bulge, characteristics that made it accessible to observers like Pierre Méchain and later catalogers such as Charles Messier and John Herschel. As M104 and NGC 4594 it features in surveys by the Sloan Digital Sky Survey, the Two Micron All Sky Survey, and the Palomar Observatory Sky Survey. Studies by teams from California Institute of Technology, Massachusetts Institute of Technology, Max Planck Society, and National Radio Astronomy Observatory have constrained its mass profile, luminosity, and environment.
Morphologically classified SA(s)a, the system shows a prominent classical bulge, an extended stellar halo, and a thin, dusty disk traced by imaging from Hubble Space Telescope and infrared data from Spitzer Space Telescope. High-resolution observations with instruments at European Southern Observatory facilities reveal a luminous central spheroid analogous to bulges in early-type spirals studied by groups at University of California, Berkeley and University of Cambridge. Radio mapping with arrays like the Very Large Array and Atacama Large Millimeter/submillimeter Array resolves cold gas and molecular complexes, while kinematic modeling by researchers at Princeton University and University of Chicago constrains the disk inclination and warp.
Distance estimates derived from planetary nebula luminosity functions, surface brightness fluctuations, and tip of the red giant branch measurements have been published by teams at Carnegie Institution for Science, University of Hawaii, and Pontificia Universidad Católica de Chile, converging near ~9.55 Mpc. Heliocentric recessional velocity measurements tied to work at Harvard–Smithsonian Center for Astrophysics and redshift catalogs from Two Micron All Sky Survey place the system at low recessional velocity within the local supercluster environment shaped by the Virgo Supercluster and interactions studied by Cosmology Research Groups at Institute for Advanced Study and CEA Saclay.
Optical spectroscopy from observatories such as Keck Observatory and Gemini Observatory and ultraviolet imaging from Galaxy Evolution Explorer show an old, metal-rich stellar population in the bulge with limited ongoing star formation in the disk, consistent with studies from University of Oxford and University of Leiden. Infrared observations by Spitzer Space Telescope and mid-infrared spectrometers operated by Jet Propulsion Laboratory detect warm dust and polycyclic aromatic hydrocarbon features indicative of low-level star formation associated with the dust lane, comparable to systems analyzed by teams at University of Toronto and Australian National University.
Multiwavelength observations from Chandra X-ray Observatory, XMM-Newton, and radio facilities like the Very Large Array reveal a low-ionization nuclear emission-line region consistent with a weak active galactic nucleus, investigated by groups at Max Planck Institute for Astrophysics and University of Edinburgh. Dynamical measurements of stellar and gas orbits using adaptive optics on telescopes at Keck Observatory and European Southern Observatory have yielded estimates for the central supermassive black hole mass, with key analyses produced by researchers at University of California, Los Angeles and Ohio State University.
Surveys with Hubble Space Telescope and ground-based imaging from Subaru Telescope and Cerro Tololo Inter-American Observatory have cataloged a rich globular cluster system, studied by teams at Yale University and University of Michigan, showing a high specific frequency compared with similar-mass spirals. Kinematic follow-up by spectrographs at Anglo-Australian Observatory and Magellan Telescopes has been used to probe the mass distribution and search for satellite dwarf galaxies akin to those cataloged by Pan-STARRS and the Sloan Digital Sky Survey.
First cataloged in the 18th and 19th centuries by observers connected to Royal Society and Paris Observatory, the object entered the Messier Catalogue and later the New General Catalogue. Imaging campaigns by teams affiliated with Mount Wilson Observatory, Palomar Observatory, and later Hubble Space Telescope programs have driven historical understanding, with analysis contributions from researchers at Smithsonian Astrophysical Observatory and Royal Astronomical Society.
The galaxy has appeared in public outreach by National Aeronautics and Space Administration and European Space Agency releases, featured in planetarium shows at institutions like the American Museum of Natural History and Griffith Observatory, and in documentary productions by BBC, Discovery Channel, and National Geographic. It is commonly used in educational materials from International Astronomical Union working groups and in imagery curated by Space Telescope Science Institute.
Category:Spiral galaxies