Sombrero Galaxy

Sombrero Galaxy
Messier 104
Observation data (J2000 epoch)
Constellation Virgo
Right ascension 12h 39m 59.4s[1]
Declination −11° 37′ 23″[1]
Redshift 0.003416±0.000017[1]
Helio radial velocity 1024±5 km/s−1[1]
Galactocentric velocity 904±7 km/s−1[1]
Distance 9.55 ± 0.31 Mpc
(31.1 ± 1.0 Mly)[2]
Absolute magnitude (B) −21.8[3]
Characteristics
Type SA(s)a;[1]
Size 15 kpc (49,000 ly)
Apparent size (V) 9′ × 4′
Notable features The overwhelming bright center
Other designations
M104, NGC 4594, UGC 293, PGC 42407

The Sombrero Galaxy (also known as Messier Object 104, M104 or NGC 4594) is a spiral galaxy[4] in the constellation Virgo located 9.55 Mpc (31,100,000 ly)[2] from Earth. The galaxy has a diameter of approximately 15kpc (50,000 light-years),[5] 30% the size of the Milky Way. It has a bright nucleus, an unusually large central bulge, and a prominent dust lane in its inclined disk. The dark dust lane and the bulge give this galaxy the appearance of a sombrero. Astronomers initially thought that the halo was small and light, indicative of a spiral galaxy, but the Spitzer Space Telescope found that the halo around the Sombrero Galaxy is larger and more massive than previously thought, indicative of a giant elliptical galaxy.[6] The galaxy has an apparent magnitude of +8.0,[5] making it easily visible with amateur telescopes, and it is considered by some authors to be the brightest galaxy within a radius of 10 megaparsecs of the Milky Way.[3] Its large bulge, its central supermassive black hole, and its dust lane all attract the attention of professional astronomers.

Observation history

Discovery

The Sombrero Galaxy[5] 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.[7][8] Charles Messier made a hand-written 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.[8] 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.[7][8] Later astronomers were able to connect Méchain's and Herschel's observations.[8]

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.[8]

Dust ring

M104 in infrared

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.[9] Most of the cold atomic hydrogen gas[10] and the dust[9] lie within this ring. The ring might also contain most of the Sombrero Galaxy's cold molecular gas,[9] although this is an inference based on observations with low resolution and weak detections.[11][12] 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.[9]

Nucleus

The nucleus of the Sombrero galaxy is classified as a low ionization nuclear emission region (LINER).[13] 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 nucleus (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.[9]

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.[14] 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 the mass of the Sun, or 109 M☉, is present in the center.[14] This is among the most massive black holes measured in any nearby galaxies.

Synchrotron radiation

At radio and X-ray wavelengths, the nucleus is a strong source of synchrotron radiation.[15][16][17][18][19][20][21] 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 nucleus. Although radio synchrotron radiation may vary over time for some active galactic nucleus, the luminosity of the radio emission from the Sombrero Galaxy varies only 10–20%.[15]

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.[9][21] 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).[9] The source of the terahertz radiation remains unidentified.

Globular clusters

The Sombrero Galaxy has a relatively large number of globular clusters. Observational studies of globular clusters in the Sombrero Galaxy have produced estimates of the population in the range of 1,200 to 2,000.[22][23][24] The ratio of the number of globular clusters to the total luminosity of the galaxy is high compared to the Milky Way and similar galaxies with small bulges, but the ratio is comparable to other galaxies with large bulges. These results have been repeatedly used to demonstrate that the number of globular clusters in galaxies is thought to be related to the size of the galaxies' bulges. The surface density of the globular clusters generally follows the light profile of the bulge except for near the center of the galaxy.[22][24][25]

Distance 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 planetary nebulae in the Sombrero Galaxy 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).[26]

The other method used is the surface brightness fluctuations method. This method uses the grainy appearance of the galaxy's bulge to estimate the distance to it. Nearby galaxy bulges will appear very grainy, while more distant bulges will appear smooth. Early measurements using this technique gave distances of 30.6 ± 1.3 Mly (9,380 ± 400 kpc).[27] Later, after some refinement of the technique, a distance of 32 ± 3 Mly (9,810 ± 920 kpc) was measured.[28] This was even further refined in 2003 to be 29.6 ± 2.5 Mly (9,080 ± 770 kpc).[29]

The average distance measured through these two techniques is 29.3 ± 1.6 Mly (8,980 ± 490 kpc).[note 1]

The absolute magnitude (in the blue) of the Sombrero Galaxy is estimated to be −21.9 at 30.6 Mly (9,400 kpc) (−21.8 at the average distance of above), that as stated above makes it the brightest galaxy within a radius of 32.6 Mly (10,000 kpc) around the Milky Way.[3]

A report from 2016 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.[30] However, it is unclear whether the Sombrero Galaxy 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.[30][31][32] However, results that rely on the percolation method (i.e. 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[33] or that it may only be part of a galaxy pair with UGCA 287.[32]

Besides that, M104 is also accompanied by an ultracompact dwarf galaxy, that was discovered in 2009. This object has an absolute magnitude of −12.3, a radius where half of its light is emitted of just 47.9 ly (3,030,000 AU), and a mass of 3.3*107 M☉[34]

Amateur astronomy

Amateur photograph of M104

The Sombrero Galaxy is located 11.5° west of Spica[8] and 5.5° northeast of Eta Corvi.[35] Although the galaxy is visible with 7x35 binoculars or a 4-inch (100 mm) amateur telescope,[35] an 8-inch (200 mm) telescope is needed to distinguish the bulge from the disk,[8] and a 10-or-12-inch (250 or 300 mm) telescope is needed to see the dark dust lane.[8]

On Jack Arnold's sci-fi 1957 feature film The Incredible Shrinking Man during Grant Williams' final voice-over, the Sombrero Galaxy is among several images that depict his thoughts on the life ahead of him, and the similarities between the infinitely large and the infinitely small.

There is also a black-and-white photograph of it in the ending credits of each and every episode of the original version of "The Outer Limits (1963 TV series)."

In the Silver Age, the hero Vartox is from a planet in the "Sombrero Hat" Galaxy.

See also

Notes

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

References

  1. 1 2 3 4 5 6 "NASA/IPAC Extragalactic Database". Results for M104. Retrieved 2008-07-09.
  2. 1 2 3 McQuinn, Kristen B. W.; Skillman, Evan D.; Dolphin, Andrew E.; Berg, Danielle; Kennicutt, Robert (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. 1 2 3 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.
  4. ↑ NASA's Sombrero Galaxy Overview and Wallpaper
  5. 1 2 3 "M 104". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-24.
  6. ↑ Famous Sombrero Galaxy Shows Surprising Side
  7. 1 2 G. R. Kepple; G. W. Sanner (1998). The Night Sky Observer's Guide. Vol. 2. Willmann-Bell. p. 451. ISBN 0-943396-60-3.
  8. 1 2 3 4 5 6 7 8 K. G. Jones (1991). Messier's Nebulae and Star Clusters (2nd ed.). Cambridge University Press. ISBN 0-521-37079-5.
  9. 1 2 3 4 5 6 7 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.
  10. ↑ 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.
  11. ↑ 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.
  12. ↑ 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.
  13. ↑ 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.
  14. 1 2 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.
  15. 1 2 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.
  16. ↑ 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.
  17. ↑ 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.
  18. ↑ 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.
  19. ↑ 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.
  20. ↑ 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.
  21. 1 2 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.
  22. 1 2 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.
  23. ↑ 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.
  24. 1 2 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.
  25. ↑ S. S. Larsen; D. A. Forbes; J. P. Brodie (2001). "Hubble Space Telescope photometry of globular clusters in the Sombrero galaxy". 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.
  26. ↑ 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.
  27. ↑ 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.
  28. ↑ 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.
  29. ↑ 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.
  30. 1 2 R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge University Press. ISBN 0-521-35299-1.
  31. ↑ P. Fouque; E. Gourgoulhon; P. Chamaraux; G. Paturel (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.
  32. 1 2 G. Giuricin; C. Marinoni; L. Ceriani; A. Pisani (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.
  33. ↑ A. Garcia (1993). "General study of group membership. II – Determination of nearby groups". Astronomy & Astrophysics. 100: 47–90. Bibcode:1993A&AS..100...47G.
  34. ↑ Hau, George K. T.; Spitler, Lee R.; Forbes, Duncan A.; Proctor, Robert N.; Strader, Jay; Mendel, J. Trevor; Brodie, Jean P.; Harris, William E. (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.
  35. 1 2 S. J. O'Meara (1998). The Messier Objects. Cambridge University Press. ISBN 0-521-55332-6.

Coordinates: 12h 39m 59.4s, −11° 37′ 23″

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