Surface brightness fluctuation

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Surface brightness fluctuation (SBF) is a secondary distance indicator used to estimate distances to galaxies. It is useful to 100 Mpc (parsec). The method measures the variance in a galaxy's light distribution arising from fluctuations in the numbers of and luminosities of individual stars per resolution element. The technique uses the fact that galaxies are made up of a finite number of stars. The number of stars in any small patch of a galaxy will vary from point to point, creating a noise-like fluctuation in its surface brightness. While the various stars present in a galaxy will cover an enormous range of luminosity, the SBF can be characterized as having an average brightness. A galaxy twice as far away appears twice as smooth as a result of the averaging. Older elliptical galaxies have fairly consistent stellar populations, thus it closely approximates a standard candle. In practice, corrections are required to account for variations in age or metallicity from galaxy to galaxy. Calibration of the method is made empirically from Cepheids or theoretically from stellar population models.

The SBF pattern is measured from the power spectrum of the residuals left behind from a deep galaxy image after a smooth model of the galaxy has been subtracted. The SBF pattern is evident as the transform of the point spread function in the Fourier domain. The amplitude of the spectrum gives the luminosity of the fluctuation star. Because the technique depends on a precise understanding of the image structure of the galaxy, extraneous sources such as globular clusters and background galaxies must be excluded. Corrections for interstellar dust absorption must also be accounted. In practice this means that SBF works best for elliptical galaxies or the bulges of S0 galaxies, and less so for spiral galaxies as they generally have complex morphologies and extensive dust features.

SBF is calibrated by use of nearby Cepheid Period-Luminosity relation (P-L) based on observations of variables located in the Large Magellanic Cloud. (Tonry 2001)(Macri 2006)

SBF is an indicator that uses stars in the old stellar populations (Population II).[1]

Notes[edit]

  1. ^ Ferrarese, Laura; Ford, Holland C.; Huchra, John; Kennicutt, Robert C., Jr.; Mould, Jeremy R.; Sakai, Shoko; Freedman, Wendy L.; Stetson, Peter B.; Madore, Barry F.; Gibson, Brad K.; Graham, John A.; Hughes, Shaun M.; Illingworth, Garth D.; Kelson, Daniel D.; Macri, Lucas; Sebo, Kim; Silbermann, N. A. (2000), "A Database of Cepheid Distance Moduli and Tip of the Red Giant Branch, Globular Cluster Luminosity Function, Planetary Nebula Luminosity Function, and Surface Brightness Fluctuation Data Useful for Distance Determinations", The Astrophysical Journal Supplement Series, 128 (2): 431–459, arXiv:astro-ph/9910501Freely accessible, Bibcode:2000ApJS..128..431F, doi:10.1086/313391. 

References[edit]

  • Tonry, John L.; Dressler, Alan; Blakeslee, John P.; Ajhar, Edward A.; Fletcher, Andre B.; Luppino, Gerard A.; Metzger, Mark R.; Moore, Christopher B. (2001), "The SBF Survey of Galaxy Distances. IV. SBF Magnitudes, Colors, and Distances", Astrophysical Journal, 546 (2): 681–693, arXiv:astro-ph/0011223Freely accessible, Bibcode:2001ApJ...546..681T, doi:10.1086/318301 
  • Macri, L. M.; Stanek, K. Z.; Bersier, D.; Greenhill, L. J.; Reid, M. J. (2006), "A New Cepheid Distance to the Maser-Host Galaxy NGC 4258 and Its Implications for the Hubble Constant", Astrophysical Journal, 652 (2): 1133–1149, arXiv:astro-ph/0608211Freely accessible, Bibcode:2006ApJ...652.1133M, doi:10.1086/508530