Stacy McGaugh
Born (1964-01-11) January 11, 1964
NationalityAmerican
Alma materMIT (S.B. 1985),
Princeton and the University of Michigan (Ph.D. 1992)
Scientific career
Fields
Institutions

Stacy McGaugh (born January 11, 1964) is an American astronomer and professor in the Department of Astronomy at Case Western Reserve University in Cleveland, Ohio. His fields of specialty include low surface brightness galaxies,[1] galaxy formation and evolution,[2] tests of dark matter[3] and alternative hypotheses,[4][5] and measurements of cosmological parameters.[6]

Stacy McGaugh was an undergraduate student at MIT (S.B. 1985) and a graduate student at Princeton and the University of Michigan (Ph.D. 1992). He held postdoctoral appointments at Cambridge University, the Carnegie Institution of Washington, and Rutgers University before joining the faculty of the University of Maryland in 1998. He moved to Case Western in 2012. He is married with two children. He is a Distinguished Alumnus of Flint (Michigan) Northern High School (2001) and of the Astronomy Department of the University of Michigan (2013).

Known in the field of extragalactic astronomy for his early work on Low Surface Brightness Galaxies[7] and the elemental abundances in HII Regions,[8] McGaugh has also contributed to the study of the kinematics of galaxies, being among the first to point out that low surface brightness galaxies are dark matter dominated and that they pose the cuspy halo problem.[9] He also coined the expression "baryonic Tully–Fisher relation.[10]" He predicted the first to second peak amplitude ratio of the acoustic power spectrum of the Cosmic microwave background radiation.[11][12] McGaugh found surprising support for the Modified Newtonian dynamics proposed by Mordehai Milgrom as an alternative to Dark matter in his work on Low Surface Brightness Galaxies.[13][14] This has proven to be very controversial since it implies the non-existence of the non-baryonic dark matter that is central to physical cosmology. Nevertheless, his predictions for the mass distribution of the Milky Way[15] and the velocity dispersions of the dwarf Spheroidal satellites of the Andromeda spiral galaxy[16] have largely been confirmed by subsequent observations.[17][18]

In 2016 McGaugh, Lelli, and Schombert reported a correlation between a radial acceleration relation (RAR) found among galactic rotation curves and the baryonic Tully-Fisher relation's prediction for galactic rotation curves.[19] According to Paranjape and Sheth, this RAR has important implications for the ΛCDM paradigm and alternative gravity theories.[20]

See also

References

  1. ↑ Bothun, G.; Impey, C.; McGaugh, S. (1997). "Low-Surface-Brightness Galaxies: Hidden Galaxies Revealed". Publications of the Astronomical Society of the Pacific. IOP Publishing. 109: 745. Bibcode:1997PASP..109..745B. doi:10.1086/133941. ISSN 0004-6280.
  2. ↑ McGaugh, S.S. (1998) "How Galaxies Don't Form"
  3. ↑ McGaugh, Stacy S.; de Blok, W. J. G. (May 20, 1998). "Testing the Dark Matter Hypothesis with Low Surface Brightness Galaxies and Other Evidence". The Astrophysical Journal. 499 (1): 41–65. arXiv:astro-ph/9801123. Bibcode:1998ApJ...499...41M. doi:10.1086/305612. ISSN 0004-637X. S2CID 16131617.
  4. ↑ Sanders, Robert H.; McGaugh, Stacy S. (2002). "Modified Newtonian Dynamics as an Alternative to Dark Matter". Annual Review of Astronomy and Astrophysics. 40 (1): 263–317. arXiv:astro-ph/0204521. Bibcode:2002ARA&A..40..263S. doi:10.1146/annurev.astro.40.060401.093923. ISSN 0066-4146. S2CID 13216648.
  5. ↑ Famaey, Benoît; McGaugh, Stacy S. (September 7, 2012). "Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions". Living Reviews in Relativity. Springer Science and Business Media LLC. 15 (1): 10. arXiv:1112.3960. Bibcode:2012LRR....15...10F. doi:10.12942/lrr-2012-10. ISSN 2367-3613. PMC 5255531. PMID 28163623.
  6. ↑ McGaugh, Stacy S. (October 1, 1999). "Distinguishing between Cold Dark Matter and Modified Newtonian Dynamics: Predictions for the Microwave Background". The Astrophysical Journal. IOP Publishing. 523 (2): L99–L102. arXiv:astro-ph/9907409. Bibcode:1999ApJ...523L..99M. doi:10.1086/312274. ISSN 0004-637X. S2CID 51842057.
  7. ↑ McGaugh, Stacy S. (1994). "Oxygen abundances in low surface brightness disk galaxies". The Astrophysical Journal. 426: 135. arXiv:astro-ph/9311064. Bibcode:1994ApJ...426..135M. doi:10.1086/174049. ISSN 0004-637X. S2CID 119364496.
  8. ↑ McGaugh, Stacy S. (1991). "H II region abundances - Model oxygen line ratios". The Astrophysical Journal. IOP Publishing. 380: 140. Bibcode:1991ApJ...380..140M. doi:10.1086/170569. ISSN 0004-637X.
  9. ↑ de Blok, W. J. G.; McGaugh, S. S.; van der Hulst, J. M. (October 21, 1996). "H I observations of low surface brightness galaxies: probing low-density galaxies". Monthly Notices of the Royal Astronomical Society. 283 (1): 18–54. arXiv:astro-ph/9605069. Bibcode:1996MNRAS.283...18D. doi:10.1093/mnras/283.1.18. ISSN 0035-8711.
  10. ↑ McGaugh, S. S.; Schombert, J. M.; Bothun, G. D.; de Blok, W. J. G. (April 20, 2000). "The Baryonic Tully-Fisher Relation". The Astrophysical Journal. IOP Publishing. 533 (2): L99–L102. arXiv:astro-ph/0003001. Bibcode:2000ApJ...533L..99M. doi:10.1086/312628. ISSN 0004-637X. PMID 10770699. S2CID 103865.
  11. ↑ McGaugh, Stacy S. (October 1, 1999). "Distinguishing between Cold Dark Matter and Modified Newtonian Dynamics: Predictions for the Microwave Background". The Astrophysical Journal. IOP Publishing. 523 (2): L99–L102. arXiv:astro-ph/9907409. Bibcode:1999ApJ...523L..99M. doi:10.1086/312274. ISSN 0004-637X. S2CID 51842057.
  12. ↑ McGaugh, Stacy S. (October 1, 2000). "Boomerang Data Suggest a Purely Baryonic Universe". The Astrophysical Journal. IOP Publishing. 541 (2): L33–L36. arXiv:astro-ph/0008188. Bibcode:2000ApJ...541L..33M. doi:10.1086/312902. ISSN 0004-637X. S2CID 51805379.
  13. ↑ McGaugh, Stacy S.; de Blok, W. J. G. (May 20, 1998). "Testing the Hypothesis of Modified Dynamics with Low Surface Brightness Galaxies and Other Evidence". The Astrophysical Journal. 499 (1): 66–81. arXiv:astro-ph/9801102. Bibcode:1998ApJ...499...66M. doi:10.1086/305629. ISSN 0004-637X. S2CID 18901029.
  14. ↑ McGaugh, Stacy S. (March 21, 2011). "Novel Test of Modified Newtonian Dynamics with Gas Rich Galaxies". Physical Review Letters. 106 (12): 121303. arXiv:1102.3913. Bibcode:2011PhRvL.106l1303M. doi:10.1103/physrevlett.106.121303. ISSN 0031-9007. PMID 21517295. S2CID 1427896.
  15. ↑ McGaugh, Stacy S. (August 10, 2008). "Milky Way Mass Models and MOND". The Astrophysical Journal. 683 (1): 137–148. arXiv:0804.1314. Bibcode:2008ApJ...683..137M. doi:10.1086/589148. ISSN 0004-637X. S2CID 16366091.
  16. ↑ McGaugh, Stacy; Milgrom, Mordehai (March 4, 2013). "Andromeda Dwarfs in Light of Modified Newtonian Dynamics". The Astrophysical Journal. 766 (1): 22. arXiv:1301.0822. Bibcode:2013ApJ...766...22M. doi:10.1088/0004-637x/766/1/22. ISSN 0004-637X. S2CID 118576979.
  17. ↑ Bovy, Jo; Rix, Hans-Walter (December 2, 2013). "A direct dynamical measurement of the Milky Way's disk surface density profile, disk scale length, and dark matter profile at 4 kpc < R < 9 kpc". The Astrophysical Journal. 779 (2): 115. arXiv:1309.0809. Bibcode:2013ApJ...779..115B. doi:10.1088/0004-637x/779/2/115. ISSN 0004-637X. S2CID 118440232.
  18. ↑ McGaugh, Stacy; Milgrom, Mordehai (September 16, 2013). "Andromeda Dwarfs in Light of MOND. II. Testing Prior Predictions". The Astrophysical Journal. 775 (2): 139. arXiv:1308.5894. Bibcode:2013ApJ...775..139M. doi:10.1088/0004-637x/775/2/139. ISSN 0004-637X. S2CID 53006824.
  19. ↑ McGaugh, Stacy S.; Lelli, Federico; Schombert, James M. (2016). "Radial Acceleration Relation in Rotationally Supported Galaxies". Physical Review Letters. 117 (20): 201101. arXiv:1609.05917. Bibcode:2016PhRvL.117t1101M. doi:10.1103/PhysRevLett.117.201101. PMID 27886485. S2CID 34521243.
  20. ↑ Paranjape, Aseem; Sheth, Ravi K. (2021). "The radial acceleration relation in a ΛCDM universe". Monthly Notices of the Royal Astronomical Society. 507: 632–650. arXiv:2102.13116. doi:10.1093/mnras/stab2141. arXiv preprint
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