Sombrero Galaxy: Difference between revisions

Sombrero Galaxy
Sombrero Galaxy
	Image taken by Hubble Space Telescope, May−June 2003
Observation data (J2000 epoch)
Constellation	Virgo
Right ascension	12h 39m 59.4314s
Declination	−11° 37′ 23.118″
Redshift	0.003416±0.000017
Heliocentric radial velocity	1,024±5 km/s
Galactocentric velocity	904±7 km/s
Distance	9.55 ± 0.31 Mpc; (31.1 ± 1.0 Mly)
Apparent magnitude (V)	8.0
Characteristics
Type	SA(s)a or E
Size	32.32 by 17.45 kiloparsecs (105,400 by 56,900 light-years); (diameter; 2MASS K-band total) ; 29.09 kiloparsecs (94,900 light-years); (diameter; D25.0 B-band isophote)
Apparent size (V)	9′ × 4′
Notable features	Unusually bright center, intriguingly detailed dust band
Other designations
	M104, IRAS 12373-1120, NGC 4594, UGCA 293, MCG -02-32-020, PGC 42407

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The Sombrero Galaxy (also known as Messier Object 104, M104^[4] or NGC 4594) is a peculiar galaxy of unclear classification^[5] in the constellation borders of Virgo and Corvus, being about 9.55 megaparsecs (31.1 million light-years)^[2] from the Milky Way galaxy. It is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster.^[6] It has an isophotal diameter of approximately 29.09 to 32.32 kiloparsecs (94,900 to 105,000 light-years),^[1] making it slightly bigger in size than the Milky Way.

It has a bright nucleus, an unusually large central bulge, and a prominent dust lane in its outer disk, which is viewed almost edge-on. The dark dust lane and the bulge give it the appearance of a sombrero hat (thus the name). Astronomers initially thought the halo was small and light, indicative of a spiral galaxy; but the Spitzer Space Telescope found that the halo was significantly larger and more massive than previously thought, indicative of a giant elliptical galaxy.^[7]

The galaxy has an apparent magnitude of +8.0,^[4] making it easily visible with amateur telescopes, and is considered by some authors to be the galaxy with the highest absolute magnitude within a radius of 10 megaparsecs of the Milky Way.^[8] Its large bulge, central supermassive black hole, and dust lane all attract the attention of professional astronomers.

Observation history

Discovery

The Sombrero Galaxy was discovered on May 11, 1781 by Pierre Méchain, who described the object in a May 1783 letter to J. Bernoulli that was later published in the Berliner Astronomisches Jahrbuch.^[9]^[10] Charles Messier made a handwritten note about this and five other objects (now collectively recognized as M104 – M109) to his personal list of objects now known as the Messier Catalogue, but it was not "officially" included until 1921.^[10] William Herschel independently discovered the object in 1784 and additionally noted the presence of a "dark stratum" in the galaxy's disc, what is now called a dust lane.^[9]^[10] Later astronomers were able to connect Méchain's and Herschel's observations.^[10]

Designation as a Messier object

In 1921, Camille Flammarion found Messier's personal list of the Messier objects including the hand-written notes about the Sombrero Galaxy. This was identified with object 4594 in the New General Catalogue, and Flammarion declared that it should be included in the Messier Catalogue. Since this time, the Sombrero Galaxy has been known as M104.^[10]

Dust ring

As noted above, this galaxy's most striking feature is the dust lane that crosses in front of the bulge of the galaxy. This dust lane is actually a symmetrical ring that encloses the bulge of the galaxy.^[11] Most of the cold atomic hydrogen gas^[12] and the dust^[11] lie within this ring. The ring might also contain most of the Sombrero Galaxy's cold molecular gas,^[11] although this is an inference based on observations with low resolution and weak detections.^[13]^[14] Additional observations are needed to confirm that the Sombrero galaxy's molecular gas is constrained to the ring. Based on infrared spectroscopy, the dust ring is the primary site of star formation within this galaxy.^[11]

Nucleus

The nucleus of the Sombrero Galaxy is classified as a low-ionization nuclear emission-line region (LINER).^[15] These are nuclear regions where ionized gas is present, but the ions are only weakly ionized (i.e. the atoms are missing relatively few electrons). The source of energy for ionizing the gas in LINERs has been debated extensively. Some LINER nuclei may be powered by hot, young stars found in star formation regions, whereas other LINER nuclei may be powered by active galactic nuclei (highly energetic regions that contain supermassive black holes). Infrared spectroscopy observations have demonstrated that the nucleus of the Sombrero Galaxy is probably devoid of any significant star formation activity. However, a supermassive black hole has been identified in the nucleus (as discussed in the subsection below), so this active galactic nucleus is probably the energy source that weakly ionizes the gas in the Sombrero Galaxy.^[11]

Central supermassive black hole

In the 1990s, a research group led by John Kormendy demonstrated that a supermassive black hole is present within the Sombrero Galaxy.^[16] Using spectroscopy data from both the CFHT and the Hubble Space Telescope, the group showed that the speed of revolution of the stars within the center of the galaxy could not be maintained unless a mass 1 billion times that of the Sun, 10⁹ M_☉, is present in the center.^[16] This is among the most massive black holes measured in any nearby galaxy, and is the nearest billion-solar-mass black hole to Earth.

Synchrotron radiation

At radio and X-ray wavelengths, the nucleus is a strong source of synchrotron radiation.^[17]^[18]^[19]^[20]^[21]^[22]^[23] Synchrotron radiation is produced when high-velocity electrons oscillate as they pass through regions with strong magnetic fields. This emission is quite common for active galactic nuclei. Although radio synchrotron radiation may vary over time for some active galactic nuclei, the luminosity of the radio emission from the Sombrero Galaxy varies only 10–20%.^[17]

Unidentified terahertz radiation

In 2006, two groups published measurements of the terahertz radiation from the nucleus of the Sombrero Galaxy at a wavelength of 850 μm.^[11]^[23] This terahertz radiation was found not to originate from the thermal emission from dust (which is commonly seen at infrared and submillimeter wavelengths), synchrotron radiation (which is commonly seen at radio wavelengths), bremsstrahlung emission from hot gas (which is uncommonly seen at millimeter wavelengths), or molecular gas (which commonly produces submillimeter spectral lines).^[11] The source of the terahertz radiation remains unidentified.

Globular clusters

The Sombrero Galaxy has a relatively large number of globular clusters, observational studies of which have produced population estimates in the range of 1,200 to 2,000.^[24]^[25]^[26] The ratio of globular clusters to the galaxy's total luminosity is high compared to the Milky Way and similar galaxies with small bulges, but comparable to other galaxies with large bulges. These results have often been used to demonstrate that the number of a galaxy's globular clusters is thought to be related to the size of its bulge. The surface density of the globular clusters generally follows the bulge's light profile, except near the galaxy's center.^[24]^[26]^[27]

Distance, mass and brightness

At least two methods have been used to measure the distance to the Sombrero Galaxy.

The first method relies on comparing the measured fluxes from the galaxy's planetary nebulae to the known luminosity of planetary nebulae in the Milky Way. This method gave the distance to the Sombrero Galaxy as 29 ± 2 Mly (8,890 ± 610 kpc).^[28]

The second method is the surface brightness fluctuations method, which uses the grainy appearance of the galaxy's bulge to estimate the distance to it. Nearby galaxy bulges appear very grainy, while more distant bulges appear smooth. Early measurements using this technique gave distances of 30.6 ± 1.3 Mly (9,380 ± 400 kpc).^[29] Later, after some refinement of the technique, a distance of 32 ± 3 Mly (9,810 ± 920 kpc) was measured.^[30] This was even further refined in 2003 to 29.6 ± 2.5 Mly (9,080 ± 770 kpc).^[31]

The average distance measured through these two techniques is 29.3 ± 1.6 Mly (8,980 ± 490 kpc).^[a]

The mass of M104 is estimated to be 800 billions solar masses^[32]

The galaxy's absolute magnitude (in the blue) is estimated as −21.9 at 30.6 Mly (9,400 kpc) (−21.8 at the average distance of above)—which, as stated above, makes it the brightest galaxy in a radius of 32.6 Mly (10,000 kpc) around the Milky Way.^[8]

A 2016 report used the Hubble Space Telescope to measure the distance to M104 based on the tip of the red-giant branch method, yielding 9.55 ± 0.13 ± 0.31 Mpc.^[2]

Nearby galaxies and galaxy group information

The Sombrero Galaxy lies within a complex, filament-like cloud of galaxies that extends to the south of the Virgo Cluster.^[33] However, it is unclear whether it is part of a formal galaxy group. Hierarchical methods for identifying groups, which determine group membership by considering whether individual galaxies belong to a larger aggregate of galaxies, typically produce results showing that the Sombrero Galaxy is part of a group that includes NGC 4487, NGC 4504, NGC 4802, UGCA 289, and possibly a few other galaxies.^[33]^[34]^[35] However, results that rely on the percolation method (also known as the friends-of-friends method), which links individual galaxies together to determine group membership, indicate that either the Sombrero Galaxy is not in a group^[36] or that it may be only part of a galaxy pair with UGCA 287.^[35]

Besides that, M104 is also accompanied by an ultra-compact dwarf galaxy, discovered in 2009, with an absolute magnitude of −12.3, an effective radius of just 47.9 ly (3.03 million astronomical units), and a mass of 3.3×10⁷ M_☉^[37]

Amateur astronomy

The Sombrero Galaxy is 11.5° west of Spica^[10] and 5.5° north-east of Eta Corvi.^[38] Although it is visible with 7×35 binoculars or a 4-inch (100 mm) amateur telescope,^[38] an 8-inch (200 mm) telescope is needed to distinguish the bulge from the disk,^[10] and a 10- or 12-inch (250 or 300 mm) telescope to see the dark dust lane.^[10]

In culture

One artistic work referencing the Sombrero Galaxy is the song South of the Sombrero Galaxy by St. Louis folk metal band Ars Arcanum. The gritty sci-fi Western piece is told from the perspective of a man on the run, from both the law and his own troubled past. The Sombrero Galaxy serves as a backdrop for the song’s narrative, blending cosmic imagery with themes of pursuit and regret.^[39]

Gallery

M104 in infrared by the Spitzer Space Telescope
Amateur photograph of M104

Notes

^ average(29.6 ± 2.5, 29 ± 2) = ((29.6 + 29) / 2) ± ((2.5² + 2²)^0.5 / 2) = 29.3 ± 1.6

References

^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j "NASA/IPAC Extragalactic Database". Results for M104. Retrieved 2008-07-09.
^ ^a ^b ^c McQuinn, Kristen B. W.; Skillman, Evan D.; Dolphin, Andrew E.; et al. (2016). "The Distance to M104". The Astronomical Journal. 152 (5): 144. arXiv:1610.03857. Bibcode:2016AJ....152..144M. doi:10.3847/0004-6256/152/5/144.
^ "Messier 104". SEDS Messier Catalog. Archived from the original on 6 October 2023. Retrieved 30 April 2022.
^ ^a ^b ^c "M 104". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-24.
^ ^a ^b "Sombrero galaxy has split personality". Science Daily. Retrieved 15 May 2022.
^ "The Virgo III Groups". Atlas of the Universe. Retrieved 2010-11-27.
^ "Famous Sombrero Galaxy Shows Surprising Side". space.com. 25 April 2012.
^ ^a ^b Karachentsev, Igor D.; Karachentseva, Valentina E.; Huchtmeier, Walter K.; Makarov, Dmitry I. (2003). "A Catalog of Neighboring Galaxies". The Astronomical Journal. 127 (4): 2031–2068. Bibcode:2004AJ....127.2031K. doi:10.1086/382905.
^ ^a ^b G. R. Kepple; G. W. Sanner (1998). The Night Sky Observer's Guide. Vol. 2. Willmann-Bell. p. 451. ISBN 978-0-943396-60-6.
^ ^a ^b ^c ^d ^e ^f ^g ^h K. G. Jones (1991). Messier's Nebulae and Star Clusters (2nd ed.). Cambridge University Press. ISBN 978-0-521-37079-0.
^ ^a ^b ^c ^d ^e ^f ^g G. J. Bendo; B. A. Buckalew; D. A. Dale; B. T. Draine; R. D. Joseph; R. C. Kennicutt Jr.; et al. (2006). "Spitzer and JCMT Observations of the Active Galactic Nucleus in the Sombrero Galaxy (NGC 4594)". The Astrophysical Journal. 645 (1): 134–147. arXiv:astro-ph/0603160. Bibcode:2006ApJ...645..134B. doi:10.1086/504033. S2CID 8027268.
^ Bajaja, E.; Van Der Burg, G.; Faber, S. M.; Gallagher, J. S.; et al. (1984). "The distribution of neutral hydrogen in the Sombrero galaxy, NGC 4594". Astronomy & Astrophysics. 141: 309–317. Bibcode:1984A&A...141..309B.
^ Bajaja, E.; Dettmar, R.-J.; Hummel, E.; Wielebinski, R. (1988). "The large-scale radio continuum structure of the Sombrero galaxy (NGC 4594)". Astronomy & Astrophysics. 202: 35–40. Bibcode:1988A&A...202...35B.
^ J. S. Young; S. Xie; L. Tacconi; P. Knezek; et al. (1995). "The FCRAO Extragalactic CO Survey. I. The Data". The Astrophysical Journal. 98: 219–257. Bibcode:1995ApJS...98..219Y. doi:10.1086/192159.
^ L. C. Ho; A. V. Filippenko; W. L. W. Sargent (1997). "A Search for "Dwarf" Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies". The Astrophysical Journal. 112 (2): 315–390. arXiv:astro-ph/9704107. Bibcode:1997ApJS..112..315H. doi:10.1086/313041. S2CID 17086638.
^ ^a ^b J. Kormendy; R. Bender; E. A. Ajhar; A.Dressler; et al. (1996). "Hubble Space Telescope Spectroscopic Evidence for a 1 X 10 9 M☉ Black Hole in NGC 4594". The Astrophysical Journal. 473 (2): L91–L94. Bibcode:1996ApJ...473L..91K. doi:10.1086/310399.
^ ^a ^b de Bruyn, A. G.; Crane, P. C.; Price, R. M.; Carlson, J. B. (1976). "The radio sources in the nuclei of NGC 3031 and NGC 4594". Astronomy & Astrophysics. 46: 243–251. Bibcode:1976A&A....46..243D.
^ Hummel, E.; van der Hulst, J. M.; Dickey, J. M. (1984). "Central radio sources in spiral galaxies – Starburst or accretion". Astronomy & Astrophysics. 134: 207–221. Bibcode:1984A&A...134..207H.
^ A. Thean; A. Pedlar; M. J. Kukula; S. A. Baum; et al. (2000). "High-resolution radio observations of Seyfert galaxies in the extended 12-μm sample - I. The observations". Monthly Notices of the Royal Astronomical Society. 314 (3): 573–588. arXiv:astro-ph/0001459. Bibcode:2000MNRAS.314..573T. doi:10.1046/j.1365-8711.2000.03401.x. S2CID 13990625.
^ T. Di Matteo; C. L. Carilli; A. C. Fabian (2001). "Limits on the Accretion Rates onto Massive Black Holes in Nearby Galaxies". The Astrophysical Journal. 547 (2): 731–739. arXiv:astro-ph/0005516. Bibcode:2001ApJ...547..731D. doi:10.1086/318405. S2CID 15963846.
^ S. Pellegrini; G. Fabbiano; F. Fiore; G. Trinchieri; et al. (2002). "Nuclear and global X-ray properties of LINER galaxies: Chandra and BeppoSAX results for Sombrero and NGC 4736". Astronomy & Astrophysics. 383 (1): 1–13. arXiv:astro-ph/0111353. Bibcode:2002A&A...383....1P. doi:10.1051/0004-6361:20011482. S2CID 16321493.
^ S. Pellegrini; A. Baldi; G. Fabbiano; D.-W. Kim (2003). "An XMM-Newton and Chandra Investigation of the Nuclear Accretion in the Sombrero Galaxy (NGC 4594)". The Astrophysical Journal. 597 (1): 175–185. arXiv:astro-ph/0307142. Bibcode:2003ApJ...597..175P. doi:10.1086/378235. S2CID 2372180.
^ ^a ^b M. Krause; R. Wielebinski; M. Dumke (2006). "Radio polarization and sub-millimeter observations of the Sombrero galaxy (NGC 4594). Large-scale magnetic field configuration and dust emission". Astronomy & Astrophysics. 448 (1): 133–142. arXiv:astro-ph/0510796. Bibcode:2006A&A...448..133K. doi:10.1051/0004-6361:20053789. S2CID 204936461.
^ ^a ^b K.-I. Wakamatsu (1977). "Radial distribution and total number of globular clusters in M104". Publications of the Astronomical Society of the Pacific. 89: 267–270. Bibcode:1977PASP...89..267W. doi:10.1086/130114. S2CID 121568307.
^ W. E. Harris; H. C. Harris; G. L. H. Harris (1984). "Globular clusters in galaxies beyond the local group. III NGC 4594 (the Sombrero)". The Astronomical Journal. 89: 216–223. Bibcode:1984AJ.....89..216H. doi:10.1086/113504.
^ ^a ^b T. J. Bridges; D. A. Hanes (1992). "The globular cluster system of NGC 4594 (the Sombrero)". The Astronomical Journal. 103: 800–814. Bibcode:1992AJ....103..800B. doi:10.1086/116102.
^ S. S. Larsen; D. A. Forbes; J. P. Brodie (2001). "Hubble Space Telescope photometry of globular clusters in the Sombrero galaxy" (PDF). Monthly Notices of the Royal Astronomical Society. 327 (4): 1116–1126. arXiv:astro-ph/0107082. Bibcode:2001MNRAS.327.1116L. doi:10.1046/j.1365-8711.2001.04797.x. S2CID 15369293.
^ H. C. Ford; X. Hui; R. Ciardullo; G. H. Jacoby; K. C. Freeman (1996). "The Stellar Halo of M104. I. A Survey for Planetary Nebulae and the Planetary Nebula Luminosity Function Distance". The Astrophysical Journal. 458: 455–466. Bibcode:1996ApJ...458..455F. doi:10.1086/176828.
^ E. A. Ajhar; T. R. Lauer; J. L. Tonry; J. P. Blakeslee; et al. (1997). "Calibration of the Surface Brightness Fluctution Method for use with the Hubble Space Telescope". The Astronomical Journal. 114: 626–634. Bibcode:1997AJ....114..626A. doi:10.1086/118498.
^ J. L. Tonry; A. Dressler; J. P. Blakeslee; E. A. Ajhar; et al. (2001). "The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances". The Astrophysical Journal. 546 (2): 681–693. arXiv:astro-ph/0011223. Bibcode:2001ApJ...546..681T. doi:10.1086/318301. S2CID 17628238.
^ Jensen, Joseph B.; Tonry, John L.; Barris, Brian J.; Thompson, Rodger I.; et al. (2003). "Measuring Distances and Probing the Unresolved Stellar Populations of Galaxies Using Infrared Surface Brightness Fluctuations". The Astrophysical Journal. 583 (2): 712–726. arXiv:astro-ph/0210129. Bibcode:2003ApJ...583..712J. doi:10.1086/345430. S2CID 551714.
^ https://science.nasa.gov/mission/hubble/science/explore-the-night-sky/hubble-messier-catalog/messier-104/
^ ^a ^b Tully, R. B. (1988). Nearby Galaxies Catalog. Cambridge University Press. ISBN 978-0-521-35299-4.
^ Fouque, P.; Gourgoulhon, E.; Chamaraux, P.; Paturel, G. (1992). "Groups of galaxies within 80 Mpc. II – The catalogue of groups and group members". Astronomy & Astrophysics. 93: 211–233. Bibcode:1992A&AS...93..211F.
^ ^a ^b Giuricin, G.; Marinoni, C.; Ceriani, L.; Pisani, A. (2000). "Nearby Optical Galaxies: Selection of the Sample and Identification of Groups". The Astrophysical Journal. 543 (1): 178–194. arXiv:astro-ph/0001140. Bibcode:2000ApJ...543..178G. doi:10.1086/317070. S2CID 9618325.
^ Garcia, A. (1993). "General study of group membership. II – Determination of nearby groups". Astronomy & Astrophysics. 100: 47–90. Bibcode:1993A&AS..100...47G.
^ Hau, George K. T.; Spitler, Lee R.; Forbes, Duncan A.; et al. (2009). "An ultra-compact dwarf around the Sombrero galaxy (M104): the nearest massive UCD". Monthly Notices of the Royal Astronomical Society: Letters. 394 (1): L97–L101. arXiv:0901.1693. Bibcode:2009MNRAS.394L..97H. doi:10.1111/j.1745-3933.2009.00618.x. S2CID 17015063.
^ ^a ^b S. J. O'Meara (1998). The Messier Objects. Cambridge University Press. ISBN 978-0-521-55332-2.
^ "South of the Sombrero Galaxy". Ars Arcanum's South of the Sombrero Galaxy on Bandcamp. Retrieved October 3, 2024.

External links

The Sombrero Galaxy on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
Hubble Mosaic of the Majestic Sombrero Galaxy (ESA)
HubbleSite: The Majestic Sombrero Galaxy (M104) Archived 2008-05-16 at the Wayback Machine
M104, the Sombrero Galaxy (NightSkyInfo.com)
Messier 104 (SEDS)
Sombrero Galaxy: A Great Observatories View
M104 The Sombrero Galaxy
Bauer, Amanda; Merrifield, Michael. "M104 – Sombrero Galaxy". Deep Sky Videos. Brady Haran.
Sombrero Galaxy (Messier 104) at Constellation Guide
South of the Sombrero Galaxy On YouTube

[average-32] verage(29.6 ± 2.5, 29 ± 2) = ((29.6 + 29) / 2) ± ((2.5² + 2²)^0.5 / 2) = 29.3 ± 1.6

[ned-1] ^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j "NASA/IPAC Extragalactic Database". Results for M104. Retrieved 2008-07-09.

[McQuinn2016-2] McQuinn, Kristen B. W.; Skillman, Evan D.; Dolphin, Andrew E.; et al. (2016). "The Distance to M104". The Astronomical Journal. 152 (5): 144. arXiv:1610.03857. Bibcode:2016AJ....152..144M. doi:10.3847/0004-6256/152/5/144.

[3] "Messier 104". SEDS Messier Catalog. Archived from the original on 6 October 2023. Retrieved 30 April 2022.

[simbad-4] "M 104". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-24.

[scidaily2012-5] "Sombrero galaxy has split personality". Science Daily. Retrieved 15 May 2022.

[atlas_universe-6] "The Virgo III Groups". Atlas of the Universe. Retrieved 2010-11-27.

[7] "Famous Sombrero Galaxy Shows Surprising Side". space.com. 25 April 2012.

[Karachentsev2004-8] Karachentsev, Igor D.; Karachentseva, Valentina E.; Huchtmeier, Walter K.; Makarov, Dmitry I. (2003). "A Catalog of Neighboring Galaxies". The Astronomical Journal. 127 (4): 2031–2068. Bibcode:2004AJ....127.2031K. doi:10.1086/382905.

[kepplesanner1998-9] G. R. Kepple; G. W. Sanner (1998). The Night Sky Observer's Guide. Vol. 2. Willmann-Bell. p. 451. ISBN 978-0-943396-60-6.

[jones1991-10] ^ ^a ^b ^c ^d ^e ^f ^g ^h K. G. Jones (1991). Messier's Nebulae and Star Clusters (2nd ed.). Cambridge University Press. ISBN 978-0-521-37079-0.

[bendoetal2006-11] ^ ^a ^b ^c ^d ^e ^f ^g G. J. Bendo; B. A. Buckalew; D. A. Dale; B. T. Draine; R. D. Joseph; R. C. Kennicutt Jr.; et al. (2006). "Spitzer and JCMT Observations of the Active Galactic Nucleus in the Sombrero Galaxy (NGC 4594)". The Astrophysical Journal. 645 (1): 134–147. arXiv:astro-ph/0603160. Bibcode:2006ApJ...645..134B. doi:10.1086/504033. S2CID 8027268.

[bajajaetal1984-12] Bajaja, E.; Van Der Burg, G.; Faber, S. M.; Gallagher, J. S.; et al. (1984). "The distribution of neutral hydrogen in the Sombrero galaxy, NGC 4594". Astronomy & Astrophysics. 141: 309–317. Bibcode:1984A&A...141..309B.

[bajajaetal1988-13] Bajaja, E.; Dettmar, R.-J.; Hummel, E.; Wielebinski, R. (1988). "The large-scale radio continuum structure of the Sombrero galaxy (NGC 4594)". Astronomy & Astrophysics. 202: 35–40. Bibcode:1988A&A...202...35B.

[youngetal1995-14] J. S. Young; S. Xie; L. Tacconi; P. Knezek; et al. (1995). "The FCRAO Extragalactic CO Survey. I. The Data". The Astrophysical Journal. 98: 219–257. Bibcode:1995ApJS...98..219Y. doi:10.1086/192159.

[hoetal1997-15] L. C. Ho; A. V. Filippenko; W. L. W. Sargent (1997). "A Search for "Dwarf" Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies". The Astrophysical Journal. 112 (2): 315–390. arXiv:astro-ph/9704107. Bibcode:1997ApJS..112..315H. doi:10.1086/313041. S2CID 17086638.

[kormendyetal1996-16] J. Kormendy; R. Bender; E. A. Ajhar; A.Dressler; et al. (1996). "Hubble Space Telescope Spectroscopic Evidence for a 1 X 10 9 M☉ Black Hole in NGC 4594". The Astrophysical Journal. 473 (2): L91–L94. Bibcode:1996ApJ...473L..91K. doi:10.1086/310399.

[debruynetal1996-17] Bruyn, A. G.; Crane, P. C.; Price, R. M.; Carlson, J. B. (1976). "The radio sources in the nuclei of NGC 3031 and NGC 4594". Astronomy & Astrophysics. 46: 243–251. Bibcode:1976A&A....46..243D.

[hummeletal1984-18] Hummel, E.; van der Hulst, J. M.; Dickey, J. M. (1984). "Central radio sources in spiral galaxies – Starburst or accretion". Astronomy & Astrophysics. 134: 207–221. Bibcode:1984A&A...134..207H.

[theanetal2000-19] A. Thean; A. Pedlar; M. J. Kukula; S. A. Baum; et al. (2000). "High-resolution radio observations of Seyfert galaxies in the extended 12-μm sample - I. The observations". Monthly Notices of the Royal Astronomical Society. 314 (3): 573–588. arXiv:astro-ph/0001459. Bibcode:2000MNRAS.314..573T. doi:10.1046/j.1365-8711.2000.03401.x. S2CID 13990625.

[dimatteoetal2001-20] T. Di Matteo; C. L. Carilli; A. C. Fabian (2001). "Limits on the Accretion Rates onto Massive Black Holes in Nearby Galaxies". The Astrophysical Journal. 547 (2): 731–739. arXiv:astro-ph/0005516. Bibcode:2001ApJ...547..731D. doi:10.1086/318405. S2CID 15963846.

[pellegrinietal2002-21] S. Pellegrini; G. Fabbiano; F. Fiore; G. Trinchieri; et al. (2002). "Nuclear and global X-ray properties of LINER galaxies: Chandra and BeppoSAX results for Sombrero and NGC 4736". Astronomy & Astrophysics. 383 (1): 1–13. arXiv:astro-ph/0111353. Bibcode:2002A&A...383....1P. doi:10.1051/0004-6361:20011482. S2CID 16321493.

[pellegrinietal2003-22] S. Pellegrini; A. Baldi; G. Fabbiano; D.-W. Kim (2003). "An XMM-Newton and Chandra Investigation of the Nuclear Accretion in the Sombrero Galaxy (NGC 4594)". The Astrophysical Journal. 597 (1): 175–185. arXiv:astro-ph/0307142. Bibcode:2003ApJ...597..175P. doi:10.1086/378235. S2CID 2372180.

[krauseetal2006-23] M. Krause; R. Wielebinski; M. Dumke (2006). "Radio polarization and sub-millimeter observations of the Sombrero galaxy (NGC 4594). Large-scale magnetic field configuration and dust emission". Astronomy & Astrophysics. 448 (1): 133–142. arXiv:astro-ph/0510796. Bibcode:2006A&A...448..133K. doi:10.1051/0004-6361:20053789. S2CID 204936461.

[wakamatsu1977-24] K.-I. Wakamatsu (1977). "Radial distribution and total number of globular clusters in M104". Publications of the Astronomical Society of the Pacific. 89: 267–270. Bibcode:1977PASP...89..267W. doi:10.1086/130114. S2CID 121568307.

[harrisetal1984-25] W. E. Harris; H. C. Harris; G. L. H. Harris (1984). "Globular clusters in galaxies beyond the local group. III NGC 4594 (the Sombrero)". The Astronomical Journal. 89: 216–223. Bibcode:1984AJ.....89..216H. doi:10.1086/113504.

[bridgeshaynes1992-26] T. J. Bridges; D. A. Hanes (1992). "The globular cluster system of NGC 4594 (the Sombrero)". The Astronomical Journal. 103: 800–814. Bibcode:1992AJ....103..800B. doi:10.1086/116102.

[27] S. S. Larsen; D. A. Forbes; J. P. Brodie (2001). "Hubble Space Telescope photometry of globular clusters in the Sombrero galaxy" (PDF). Monthly Notices of the Royal Astronomical Society. 327 (4): 1116–1126. arXiv:astro-ph/0107082. Bibcode:2001MNRAS.327.1116L. doi:10.1046/j.1365-8711.2001.04797.x. S2CID 15369293.

[fordetal1996-28] H. C. Ford; X. Hui; R. Ciardullo; G. H. Jacoby; K. C. Freeman (1996). "The Stellar Halo of M104. I. A Survey for Planetary Nebulae and the Planetary Nebula Luminosity Function Distance". The Astrophysical Journal. 458: 455–466. Bibcode:1996ApJ...458..455F. doi:10.1086/176828.

[ajharetal1997-29] E. A. Ajhar; T. R. Lauer; J. L. Tonry; J. P. Blakeslee; et al. (1997). "Calibration of the Surface Brightness Fluctution Method for use with the Hubble Space Telescope". The Astronomical Journal. 114: 626–634. Bibcode:1997AJ....114..626A. doi:10.1086/118498.

[tonryetal2001-30] J. L. Tonry; A. Dressler; J. P. Blakeslee; E. A. Ajhar; et al. (2001). "The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances". The Astrophysical Journal. 546 (2): 681–693. arXiv:astro-ph/0011223. Bibcode:2001ApJ...546..681T. doi:10.1086/318301. S2CID 17628238.

[jensenetal2003-31] Jensen, Joseph B.; Tonry, John L.; Barris, Brian J.; Thompson, Rodger I.; et al. (2003). "Measuring Distances and Probing the Unresolved Stellar Populations of Galaxies Using Infrared Surface Brightness Fluctuations". The Astrophysical Journal. 583 (2): 712–726. arXiv:astro-ph/0210129. Bibcode:2003ApJ...583..712J. doi:10.1086/345430. S2CID 551714.

[33] ttps://science.nasa.gov/mission/hubble/science/explore-the-night-sky/hubble-messier-catalog/messier-104/

[nbg-34] Tully, R. B. (1988). Nearby Galaxies Catalog. Cambridge University Press. ISBN 978-0-521-35299-4.

[fouqueetal1992-35] Fouque, P.; Gourgoulhon, E.; Chamaraux, P.; Paturel, G. (1992). "Groups of galaxies within 80 Mpc. II – The catalogue of groups and group members". Astronomy & Astrophysics. 93: 211–233. Bibcode:1992A&AS...93..211F.

[giuricinetal2002-36] Giuricin, G.; Marinoni, C.; Ceriani, L.; Pisani, A. (2000). "Nearby Optical Galaxies: Selection of the Sample and Identification of Groups". The Astrophysical Journal. 543 (1): 178–194. arXiv:astro-ph/0001140. Bibcode:2000ApJ...543..178G. doi:10.1086/317070. S2CID 9618325.

[garcia1993-37] Garcia, A. (1993). "General study of group membership. II – Determination of nearby groups". Astronomy & Astrophysics. 100: 47–90. Bibcode:1993A&AS..100...47G.

[Hau2009-38] Hau, George K. T.; Spitler, Lee R.; Forbes, Duncan A.; et al. (2009). "An ultra-compact dwarf around the Sombrero galaxy (M104): the nearest massive UCD". Monthly Notices of the Royal Astronomical Society: Letters. 394 (1): L97–L101. arXiv:0901.1693. Bibcode:2009MNRAS.394L..97H. doi:10.1111/j.1745-3933.2009.00618.x. S2CID 17015063.

[omeara1998-39] S. J. O'Meara (1998). The Messier Objects. Cambridge University Press. ISBN 978-0-521-55332-2.

[40] "South of the Sombrero Galaxy". Ars Arcanum's South of the Sombrero Galaxy on Bandcamp. Retrieved October 3, 2024.

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[2]

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[5]

[6]

[7]

[8]

[9]

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[11]

[12]

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[14]

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[39]

@@ Line 4: / Line 4: @@
 | name               = Sombrero Galaxy
 | image              = File:M104_ngc4594_sombrero_galaxy_hi-res.jpg
-| image_size         = 310px
 | caption            = Image taken by [[Hubble Space Telescope]], May−June 2003
 | epoch              = [[Epoch (astronomy)#Julian years and J2000|J2000]]
 | constellation name = [[Virgo (constellation)|Virgo]]
-| ra                 = {{RA|12|39|59.4}}<ref name="ned"/>
+| ra                 = {{RA|12|39|59.4314}}<ref name="ned"/>
-| dec                = {{DEC|-11|37|23}}<ref name="ned"/>
+| dec                = {{DEC|-11|37|23.118}}<ref name="ned"/>
 | z                  = {{val|0.003416|0.000017|fmt=none}}<ref name="ned"/>
 | h_radial_v         = {{val|1024|5|u=km/s|fmt=commas}}<ref name="ned"/>
@@ Line 16: / Line 15: @@
 | group_cluster      =
 | type               = SA(s)a<ref name="ned">{{cite web |title=NASA/IPAC Extragalactic Database |work=Results for M104 |url=http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=M104&extend=no&out_csys=Equatorial&out_equinox=J2000.0&obj_sort=RA+or+Longitude&of=pre_text&zv_breaker=30000.0&list_limit=5&img_stamp=YES |access-date=2008-07-09}}</ref> or E<ref name="scidaily2012">{{cite news |title=Sombrero galaxy has split personality|url=https://www.sciencedaily.com/releases/2012/04/120424161412.htm |access-date=15 May 2022 |newspaper=Science Daily}}</ref>
-| size               = {{cvt|32.32|x|17.45|kpc|kly|sigfig=4|abbr=on|lk=on|disp=x|<br />(|)}}<br />{{small|(''[[Galaxy#Isophotal diameter|diameter]]; [[2MASS]] K-band total isophote'')}}<ref name=ned/>
+| size               = {{convert|32.32|x|17.45|kpc|ly|-2|abbr=off|lk=on}}<br />([[Galaxy#Isophotal diameter|diameter]]; [[2MASS]] K-band total)<ref name=ned/>
-<br />{{cvt|29.09|kpc|kly|sigfig=4|abbr=on|lk=on|disp=x| (|)}}<br />{{small|(''[[Galaxy#Isophotal diameter|diameter]]; D<sub>25.0</sub> B-band isophote'')}}<ref name=ned/>
+<br />{{convert|29.09|kpc|ly|-2|abbr=off|lk=on}}<br />([[Galaxy#Isophotal diameter|diameter]]; D<sub>25.0</sub> B-band isophote)<ref name=ned/>
 | stars              =
 | appmag_v           = 8.0<ref>{{cite web |url=https://messier.seds.org/m/m104.html |title=Messier 104 |access-date=30 April 2022 |website=SEDS Messier Catalog |archive-date=6 October 2023 |archive-url=https://web.archive.org/web/20231006225339/http://www.messier.seds.org/m/m104.html |url-status=dead }}</ref><ref name= "simbad">{{cite simbad |title=M 104
 |access-date=2017-09-24}}</ref>
 | absmag_v           =
-| absmag_b           = −21.8<ref name="Karachentsev2004"/>
 | size_v             = {{val|9|x|4|ul=arcminute}}<ref name="ned"/>
 | notes              = Unusually bright center, intriguingly detailed dust band
-| names              = [[Messier object|M]]104, [[New General Catalogue|NGC]]&nbsp;4594, [[Uppsala General Catalogue|UGC]]&nbsp;293, [[Principal Galaxies Catalogue|PGC]]&nbsp;42407
+| names              = {{odlist | name = [[Messier object|M]]104 | NGC= 4594 | UGCA= 293 | PGC= 42407 | MCG= -02-32-020 | IRAS= 12373-1120}}
 | references         =
 }}
@@ Line 42: / Line 40: @@
 ==Dust ring==
-[[File:Sombrero Galaxy in infrared (Ssc2005-11a3).jpg|thumb|M104 in infrared]]
+[[Image:Sombrero Galaxy (MIRI Image) (2024-137).png|thumb|M104 captured by the [[James Webb Space Telescope]]'s [[Mid-Infrared Instrument]] in 2024.]]
 As noted above, this galaxy's most striking feature is the [[dust lane]] that crosses in front of the bulge of the galaxy. This dust lane is actually a symmetrical ring that encloses the bulge of the galaxy.<ref name="bendoetal2006">{{cite journal |author=G. J. Bendo |author2=B. A. Buckalew |author3=D. A. Dale |author4=B. T. Draine |author5=R. D. Joseph |author6=R. C. Kennicutt Jr. |author7=K. Sheth |author8=J.-D. T. Smith |author9=F. Walter | author10= D. Calzetti |author11=J. M. Cannon |author12=C. W. Engelbracht |author13=K. D. Gordon |author14=G. Helou |author15=D. Hollenbach |author16=E. J. Murphy |author17=H. Roussel |display-authors=6 |date=2006 |title=Spitzer and JCMT Observations of the Active Galactic Nucleus in the Sombrero Galaxy (NGC 4594) |journal=[[The Astrophysical Journal]] |volume=645 |issue=1 |pages=134–147 |bibcode=2006ApJ...645..134B |doi=10.1086/504033 |arxiv=astro-ph/0603160|s2cid=8027268 }}</ref> Most of the cold atomic hydrogen gas<ref name="bajajaetal1984">{{cite journal |last1=Bajaja |first1=E. |display-authors=4 |last2=Van Der Burg |first2=G. |last3=Faber |first3=S. M. |last4=Gallagher |first4=J. S. |last5=Knapp |first5=G. R. |last6=Shane |first6=W. W. |date=1984 |title=The distribution of neutral hydrogen in the Sombrero galaxy, NGC 4594 |journal=[[Astronomy & Astrophysics]] |volume=141 |pages=309–317 |bibcode=1984A&A...141..309B}}</ref> and the dust<ref name="bendoetal2006"/> lie within this ring. The ring might also contain most of the Sombrero Galaxy's cold molecular gas,<ref name="bendoetal2006"/> although this is an inference based on observations with low resolution and weak detections.<ref name="bajajaetal1988">{{cite journal |last1=Bajaja |first1=E. |last2=Dettmar |first2=R.-J. |last3=Hummel |first3=E. |last4=Wielebinski |first4=R. |date=1988 |title=The large-scale radio continuum structure of the Sombrero galaxy (NGC 4594) |journal=[[Astronomy & Astrophysics]] |volume=202 |pages=35–40 |bibcode=1988A&A...202...35B}}</ref><ref name="youngetal1995">{{cite journal |author=J. S. Young |display-authors=4 |author2=S. Xie |author3=L. Tacconi |author4=P. Knezek |author5=P. Viscuso |author6=L. Tacconi-Garman |author7=N. Scoville |author8=S. Schneider |author9=F. P. Schloerb | author10= S. Lord |author11=A. Lesser |author12=J. Kenney |author13=Y.-L. Huang |author14=N. Devereux |author15=M. Claussen |author16=J. Case |author17=J. Carpenter |author18=M. Berry |author19=L. Allen |date=1995 |title=The FCRAO Extragalactic CO Survey. I. The Data |journal=[[The Astrophysical Journal]] |volume=98 |pages=219–257 |bibcode=1995ApJS...98..219Y |doi=10.1086/192159|doi-access=free }}</ref> Additional observations are needed to confirm that the Sombrero galaxy's molecular gas is constrained to the ring. Based on [[infrared]] [[spectroscopy]], the dust ring is the primary site of star formation within this galaxy.<ref name="bendoetal2006"/>
@@ Line 61: / Line 59: @@
 The Sombrero Galaxy has a relatively large number of [[globular cluster]]s, observational studies of which have produced population estimates in the range of 1,200 to 2,000.<ref name="wakamatsu1977">{{cite journal |author=K.-I. Wakamatsu |date=1977 |title=Radial distribution and total number of globular clusters in M104 |journal=[[Publications of the Astronomical Society of the Pacific]] |volume=89 |pages=267–270 |bibcode=1977PASP...89..267W |doi=10.1086/130114|s2cid=121568307 |doi-access=free }}</ref><ref name="harrisetal1984">{{cite journal |author=W. E. Harris |author2=H. C. Harris |author3=G. L. H. Harris |date=1984 |title=Globular clusters in galaxies beyond the local group. III NGC 4594 (the Sombrero) |journal=[[The Astronomical Journal]] |volume=89 |pages=216–223 |bibcode=1984AJ.....89..216H |doi=10.1086/113504|doi-access=free }}</ref><ref name="bridgeshaynes1992">{{cite journal |author=T. J. Bridges |author2=D. A. Hanes |date=1992 |title=The globular cluster system of NGC 4594 (the Sombrero) |journal=[[The Astronomical Journal]] |volume=103 |pages=800–814 |bibcode=1992AJ....103..800B |doi=10.1086/116102|doi-access=free }}</ref> The ratio of globular clusters to the galaxy's total luminosity is high compared to the [[Milky Way]] and similar galaxies with small bulges, but comparable to other galaxies with large bulges. These results have often been used to demonstrate that the number of a galaxy's globular clusters is thought to be related to the size of its bulge. The surface density of the globular clusters generally follows the bulge's light profile, except near the galaxy's center.<ref name="wakamatsu1977"/><ref name="bridgeshaynes1992"/><ref>{{cite journal |author=S. S. Larsen |author2=D. A. Forbes |author3=J. P. Brodie |date=2001 |title=Hubble Space Telescope photometry of globular clusters in the Sombrero galaxy |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=327 |issue=4 |pages=1116–1126 |bibcode=2001MNRAS.327.1116L |doi=10.1046/j.1365-8711.2001.04797.x |doi-access=free |arxiv=astro-ph/0107082|s2cid=15369293 |url=https://researchbank.swinburne.edu.au/file/930d5c03-c31e-437b-8475-b9496b44f13a/1/PDF%20(Accepted%20manuscript).pdf }}</ref>
-==Distance and brightness==
+==Distance, mass and brightness==
 At least two methods have been used to measure the distance to the Sombrero Galaxy.
@@ Line 69: / Line 67: @@
 The average distance measured through these two techniques is {{cvt|29.3|±|1.6|Mly}}.{{efn|name=average|reference= average(29.6 ± 2.5, 29 ± 2) = ((29.6 + 29) / 2) ± ((2.5<sup>2</sup> + 2<sup>2</sup>)<sup>0.5</sup> / 2) = 29.3 ± 1.6}}
+The mass of M104 is estimated to be 800 billions solar masses<ref>https://science.nasa.gov/mission/hubble/science/explore-the-night-sky/hubble-messier-catalog/messier-104/</ref>
 The galaxy's [[absolute magnitude]] (in the blue) is estimated as −21.9 at {{cvt|30.6|Mly}} (−21.8 at the average distance of above)—which, as stated above, makes it the brightest galaxy in a radius of {{cvt|32.6|Mly}} around the Milky Way.<ref name="Karachentsev2004"/>
@@ Line 75: / Line 75: @@
 ==Nearby galaxies and galaxy group information==
-The Sombrero Galaxy lies within a complex, [[Galaxy filament|filament]]-like cloud of galaxies that extends to the south of the [[Virgo Cluster]].<ref name="nbg">{{cite book |first=R. B. | last= Tully |date=1988 |title=Nearby Galaxies Catalog |publisher=[[Cambridge University Press]] |isbn=978-0-521-35299-4}}</ref> However, it is unclear whether it is part of a formal [[galaxy group]]. Hierarchical methods for identifying groups, which determine group membership by considering whether individual galaxies belong to a larger aggregate of galaxies, typically produce results showing that the Sombrero Galaxy is part of a group that includes NGC 4487, NGC 4504, NGC 4802, UGCA 289, and possibly a few other galaxies.<ref name="nbg"/><ref name="fouqueetal1992">{{cite journal |first1=P. | last1= Fouque | first2=E. | last2= Gourgoulhon | first3=P. | last3= Chamaraux |first4=G. | last4=Paturel |date=1992 |title=Groups of galaxies within 80 Mpc. II – The catalogue of groups and group members |journal=[[Astronomy & Astrophysics]] |volume=93 |pages=211–233 |bibcode=1992A&AS...93..211F}}</ref><ref name="giuricinetal2002">{{cite journal |first1= G. |last1= Giuricin |first2= C. |last2= Marinoni |first3= L. |last3= Ceriani |first4= A. |last4= Pisani |date=2000 |title= Nearby Optical Galaxies: Selection of the Sample and Identification of Groups |journal=[[The Astrophysical Journal]] |volume=543 |issue=1 |pages=178–194 |bibcode= 2000ApJ...543..178G |doi=10.1086/317070 |arxiv=astro-ph/0001140|s2cid= 9618325 }}</ref> However, results that rely on the [[Percolation theory|percolation]] method (also known as the friends-of-friends method), which links individual galaxies together to determine group membership, indicate that either the Sombrero Galaxy is not in a group<ref name="garcia1993">{{cite journal |first=A. | last= Garcia |date=1993 |title=General study of group membership. II – Determination of nearby groups |journal= Astronomy & Astrophysics |volume=100 |pages=47–90 |bibcode= 1993A&AS..100...47G}}</ref> or that it may be only part of a galaxy pair with [[UGCA 287]].<ref name="giuricinetal2002"/>
+The Sombrero Galaxy lies within a complex, [[Galaxy filament|filament]]-like cloud of galaxies that extends to the south of the [[Virgo Cluster]].<ref name="nbg">{{cite book |first=R. B. | last= Tully |date=1988 |title=Nearby Galaxies Catalog |publisher=[[Cambridge University Press]] |isbn=978-0-521-35299-4}}</ref> However, it is unclear whether it is part of a formal [[galaxy group]]. Hierarchical methods for identifying groups, which determine group membership by considering whether individual galaxies belong to a larger aggregate of galaxies, typically produce results showing that the Sombrero Galaxy is part of a group that includes [[NGC 4487]], [[NGC 4504]], [[NGC 4802]], [[UGCA 289]], and possibly a few other galaxies.<ref name="nbg"/><ref name="fouqueetal1992">{{cite journal |first1=P. | last1= Fouque | first2=E. | last2= Gourgoulhon | first3=P. | last3= Chamaraux |first4=G. | last4=Paturel |date=1992 |title=Groups of galaxies within 80 Mpc. II – The catalogue of groups and group members |journal=[[Astronomy & Astrophysics]] |volume=93 |pages=211–233 |bibcode=1992A&AS...93..211F}}</ref><ref name="giuricinetal2002">{{cite journal |first1= G. |last1= Giuricin |first2= C. |last2= Marinoni |first3= L. |last3= Ceriani |first4= A. |last4= Pisani |date=2000 |title= Nearby Optical Galaxies: Selection of the Sample and Identification of Groups |journal=[[The Astrophysical Journal]] |volume=543 |issue=1 |pages=178–194 |bibcode= 2000ApJ...543..178G |doi=10.1086/317070 |arxiv=astro-ph/0001140|s2cid= 9618325 }}</ref> However, results that rely on the [[Percolation theory|percolation]] method (also known as the friends-of-friends method), which links individual galaxies together to determine group membership, indicate that either the Sombrero Galaxy is not in a group<ref name="garcia1993">{{cite journal |first=A. | last= Garcia |date=1993 |title=General study of group membership. II – Determination of nearby groups |journal= Astronomy & Astrophysics |volume=100 |pages=47–90 |bibcode= 1993A&AS..100...47G}}</ref> or that it may be only part of a galaxy pair with [[UGCA 287]].<ref name="giuricinetal2002"/>
 Besides that, M104 is also accompanied by an [[ultra-compact dwarf galaxy]], discovered in 2009, with an [[absolute magnitude]] of −12.3, an [[effective radius]] of just {{convert|47.9|ly|abbr=in|e6AU|lk=out}}, and a mass of 3.3×{{solar mass|10<sup>7</sup>|link=on}}<ref name="Hau2009">{{cite journal | display-authors = 3| author1=Hau, George K. T. |author2=Spitler, Lee R. |author3=Forbes, Duncan A. |author4=Proctor, Robert N. |author5=Strader, Jay |author6=Mendel, J. Trevor |author7=Brodie, Jean P. |author8= Harris, William E. |title=An ultra-compact dwarf around the Sombrero galaxy (M104): the nearest massive UCD |journal=Monthly Notices of the Royal Astronomical Society: Letters |date=2009 |volume=394 |issue=1 |pages=L97–L101 |bibcode= 2009MNRAS.394L..97H |doi=10.1111/j.1745-3933.2009.00618.x | doi-access=free |arxiv= 0901.1693|s2cid=17015063 }}</ref>
 ==Amateur astronomy==
-[[File:Sombrero Galaxy (also known as Messier Object 104, M104 or NGC 4594) (cropped).jpg|thumb|Amateur photograph of M104]]
 The Sombrero Galaxy is 11.5° west of [[Spica]]<ref name="jones1991"/> and 5.5° north-east of [[Eta Corvi]].<ref name="omeara1998">{{cite book |author=S. J. O'Meara |date=1998 |title=The Messier Objects |publisher=[[Cambridge University Press]] |isbn=978-0-521-55332-2 |url-access=registration |url=https://archive.org/details/messierobjectsfi00omea }}</ref> Although it is visible with 7×35 [[binoculars]] or a {{convert|4|in|adj=on}} amateur telescope,<ref name="omeara1998"/> an {{convert|8|in|adj=on}} telescope is needed to distinguish the bulge from the disk,<ref name="jones1991"/> and a 10- or 12-inch (250 or 300&nbsp;mm) telescope to see the dark dust lane.<ref name="jones1991"/>
+==In culture==
+One artistic work referencing the Sombrero Galaxy is the song ''South of the Sombrero Galaxy'' by St. Louis folk metal band Ars Arcanum. The gritty sci-fi Western piece is told from the perspective of a man on the run, from both the law and his own troubled past. The Sombrero Galaxy serves as a backdrop for the song’s narrative, blending cosmic imagery with themes of pursuit and regret.<ref>{{cite web | title=South of the Sombrero Galaxy | url=https://arsarcanum.bandcamp.com/track/south-of-the-sombrero-galaxy | website=Ars Arcanum's South of the Sombrero Galaxy on Bandcamp | access-date=October 3, 2024}}</ref>
+== Gallery ==
+<gallery widths="300">
+File:Sombrero Galaxy in infrared (Ssc2005-11a3).jpg|M104 in infrared by the Spitzer Space Telescope
+File:Sombrero Galaxy (also known as Messier Object 104, M104 or NGC 4594) (cropped).jpg|Amateur photograph of M104
+</gallery>
 ==See also==
@@ Line 114: / Line 123: @@
 * {{cite web |last=Bauer |first=Amanda |title=M104 – Sombrero Galaxy |url=http://www.deepskyvideos.com/videos/messier/M104_sombrero_galaxy.html |work=Deep Sky Videos |publisher=[[Brady Haran]] |author2=Merrifield, Michael}}
 * [http://www.constellation-guide.com/sombrero-galaxy-messier-104/ Sombrero Galaxy (Messier 104) at Constellation Guide]
+* [https://www.youtube.com/watch?v=8zOtfrVpDpk South of the Sombrero Galaxy On YouTube]
 {{Messier objects}}
@@ Line 121: / Line 131: @@
 {{Portal bar|Astronomy|Stars|Outer space}}
 {{Authority control}}
-{{Sky|12|39|59.4|-|11|37|23|29300000}}
+{{Sky|12|39|59.4314|-|11|37|23.118|29300000}}
 {{DEFAULTSORT:Sombrero Galaxy}}
@@ Line 130: / Line 140: @@
 [[Category:Messier objects]]
 [[Category:NGC objects]]
-[[Category:Principal Galaxies Catalogue objects|42407]]
+[[Category:Principal Galaxies Catalogue objects|042407]]
 [[Category:Astronomical objects discovered in 1781|17810511]]
 [[Category:Discoveries by Pierre Méchain]]
 [[Category:Peculiar galaxies]]
-[[Category:UGCA objects]]
+[[Category:UGCA objects|293]]
+[[Category:IRAS catalogue objects|12373-1120]]
+[[Category:MCG objects|-02-32-020]]

v t e Messier objects
List	M1 M2 M3 M4 M5 M6 M7 M8 M9 M10 M11 M12 M13 M14 M15 M16 M17 M18 M19 M20 M21 M22 M23 M24 M25 M26 M27 M28 M29 M30 M31 M32 M33 M34 M35 M36 M37 M38 M39 M40 M41 M42 M43 M44 M45 M46 M47 M48 M49 M50 M51 M52 M53 M54 M55 M56 M57 M58 M59 M60 M61 M62 M63 M64 M65 M66 M67 M68 M69 M70 M71 M72 M73 M74 M75 M76 M77 M78 M79 M80 M81 M82 M83 M84 M85 M86 M87 M88 M89 M90 M91 M92 M93 M94 M95 M96 M97 M98 M99 M100 M101 M102 M103 Added M104 M105 M106 M107 M108 M109 M110
See also	Caldwell catalogue Catalogue of Nebulae and Clusters of Stars Herschel 400 Catalogue Index Catalogue New General Catalogue Revised New General Catalogue
Category Commons Portal

v t e Astronomical catalogs
Messier	M95 M96 M97 M98 M99 M100 M101 M102 M103 M104 M105 M106 M107 M108 M109 M110
NGC	NGC 4589 NGC 4590 NGC 4591 NGC 4592 NGC 4593 NGC 4594 NGC 4595 NGC 4596 NGC 4597 NGC 4598 NGC 4599
PGC	PGC 42403 PGC 42404 PGC 42405 PGC 42406 PGC 42407 PGC 42408 PGC 42409 PGC 42410 PGC 42411
UGC	UGC 289 UGC 290 UGC 291 UGC 292 UGC 293 UGC 294 UGC 295 UGC 296 UGC 297
GC	GC 3127 GC 3128 GC 3129 GC 3130 GC 3131 GC 3132 GC 3133 GC 3134 GC 3135 GC 3136 GC 3137