Messier 108

Messier 108
A Sloan Digital Sky Survey image of M108.
Observation data (J2000 epoch)
ConstellationUrsa Major[1]
Right ascension11h 11m 31.0s[2]
Declination+55° 40′ 27″[2]
Redshift696.1 ± 0.6 km/s[2]
Distance8.8 Mpc (28.7 Mly) [3]
Apparent magnitude (V)10.0[4]
Characteristics
TypeSB(s)cd[5]
Apparent size (V)8′.7 × 2′.2[2]
Other designations
NGC 3556,[2] PGC 34030,[2] UGC 6225[2]
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Messier 108 (also known as NGC 3556, nicknamed the Surfboard Galaxy[6]) is a barred spiral galaxy about 28 million light-years away from Earth[3] in the northern constellation Ursa Major. It was discovered by Pierre Méchain in 1781 or 1782.[7] From the Earth, this galaxy is seen almost edge-on.

This galaxy is an isolated[8] member of the Ursa Major Cluster of galaxies in the local supercluster. It has a morphological classification of type SBbc in the de Vaucouleurs system, which means it is a barred spiral galaxy with somewhat loosely wound arms. The maximum angular size of the galaxy in the optical band is 11′.1 × 4′.6, and it is inclined 75° to the line of sight.[5]

This galaxy has an estimated mass of 125 billion solar masses (M☉)[9][note 1] and bears about 290 ± 80 globular clusters.[9] Examination of the distribution of neutral hydrogen in this galaxy shows discrete shells of expanding gas extending for several kiloparsecs, known as H1 supershells. These may be driven by currents of dark matter, dust and gas contributing to large star formation, having caused supernovae explosions. Alternatively they may result from an infall from the intergalactic medium or arise from radio jets.[10]

Observations with the Chandra X-ray Observatory have identified 83 X-ray sources, including a source at the nucleus. The brightest of these is consistent with an intermediate-mass black hole accreting matter. The galaxy is also emitting a diffuse soft X-ray radiation within 2.6 arcminutes of the optical galaxy.[8][note 2] The spectrum of the source at the core is consistent with an active galactic nucleus, but an examination with the Spitzer Space Telescope showed no indication of activity. The supermassive black hole at the core has an estimated mass of 24 million solar masses (M☉).[11]

  1. ^ R. W. Sinnott, ed. (1988). The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer. Sky Publishing Corporation/Cambridge University Press. ISBN 978-0-933346-51-2.
  2. ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 3556. Retrieved 30 March 2022.
  3. ^ a b c Sorce, J. G.; et al. (2014). "From Spitzer Galaxy photometry to Tully–Fisher distances". Monthly Notices of the Royal Astronomical Society. 444 (1): 527–541. arXiv:1408.0729. doi:10.1093/mnras/stu1450.
  4. ^ "Messier 108". SEDS Messier Catalog. Retrieved 30 April 2022.
  5. ^ a b Tully, R. B.; Fisher, J. R. (1977). "A new method of determining distances to galaxies". Astronomy and Astrophysics. 54 (3): 661–673. Bibcode:1977A&A....54..661T.
  6. ^ Cite error: The named reference guide was invoked but never defined (see the help page).
  7. ^ Kepple, George Robert; Glen W. Sanner (1998). The Night Sky Observer's Guide. Vol. 2. Willmann-Bell. p. 399. ISBN 978-0-943396-60-6.
  8. ^ a b c Wang, Q. Daniel; et al. (2003). "Chandra Observation of the Edge-on Galaxy NGC 3556 (M 108): Violent Galactic Disk-halo Interaction Revealed". The Astrophysical Journal. 598 (2): 969–981. arXiv:astro-ph/0308150. Bibcode:2003ApJ...598..969W. doi:10.1086/379010. S2CID 49349099.
  9. ^ a b Rhode, Katherine L.; et al. (2007). "Global Properties of the Globular Cluster Systems of Four Spiral Galaxies". Astronomical Journal. 134 (4): 1403–1418. arXiv:0708.1166. Bibcode:2007AJ....134.1403R. doi:10.1086/521397. S2CID 15834447.
  10. ^ Gopal-Krishna; Irwin, Judith A. (2000). "Radio jet-blown neutral hydrogen supershells in spiral galaxies?". Astronomy and Astrophysics. 361: 888–894. arXiv:astro-ph/0008251. Bibcode:2000A&A...361..888G.
  11. ^ Satyapal, S.; et al. (2008). "Spitzer Uncovers Active Galactic Nuclei Missed by Optical Surveys in Seven Late-Type Galaxies". Astrophysical Journal. 677 (2): 926–942. arXiv:0801.2759. Bibcode:2008ApJ...677..926S. doi:10.1086/529014. S2CID 16050838.


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