SigSpec

Short description: Statistical technique

SigSpec (acronym of SIGnificance SPECtrum) is a statistical technique to provide the reliability of periodicities in a measured (noisy and not necessarily equidistant) time series. It relies on the amplitude spectrum obtained by the Discrete Fourier transform (DFT) and assigns a quantity called the spectral significance (frequently abbreviated by “sig”) to each amplitude. This quantity is a logarithmic measure of the probability that the given amplitude level would be seen in white noise, in the sense of a type I error. It represents the answer to the question, “What would be the chance to obtain an amplitude like the measured one or higher, if the analysed time series were random?”

SigSpec may be considered a formal extension to the Lomb-Scargle periodogram, appropriately incorporating a time series to be averaged to zero before applying the DFT, which is done in many practical applications. When a zero-mean corrected dataset has to be statistically compared to a random sample, the sample mean (rather than the population mean only) has to be zero.

Probability density function (pdf) of white noise in Fourier space

Considering a time series to be represented by a set of [math]\displaystyle{ K }[/math] pairs [math]\displaystyle{ (t_k,x_k) }[/math], the amplitude pdf of white noise in Fourier space, depending on frequency and phase angle may be described in terms of three parameters, [math]\displaystyle{ \alpha_0 }[/math], [math]\displaystyle{ \beta_0 }[/math], [math]\displaystyle{ \theta_0 }[/math], defining the “sampling profile”, according to

[math]\displaystyle{ \tan 2\theta_0 = \frac{K\sum_{k=0}^{K-1}\sin 2\omega t_k - 2\left(\sum_{k=0}^{K-1}\cos\omega t_k\right)\left(\sum_{k=0}^{K-1}\sin\omega t_k\right)}{K\sum_{k=0}^{K-1}\cos 2\omega t_k - \big(\sum_{k=0}^{K-1}\cos\omega t_k\big)^2 + \big(\sum_{k=0}^{K-1}\sin\omega t_k\big)^2}, }[/math]

[math]\displaystyle{ \alpha_0 = \sqrt{\frac{2}{K^2}\left( K\sum_{k=0}^{K-1}\cos ^2\left(\omega t_k-\theta_0\right) -\left[\sum_{l=0}^{K-1}\cos\left(\omega t_k-\theta_0\right)\right]^2\right)}, }[/math]

[math]\displaystyle{ \beta_0 = \sqrt{\frac{2}{K^2}\left( K\sum_{k=0}^{K-1}\sin ^2\left(\omega t_k-\theta_0\right) -\left[\sum_{l=0}^{K-1}\sin\left(\omega t_k-\theta_0\right)\right]^2\right)}. }[/math]

In terms of the phase angle in Fourier space, [math]\displaystyle{ \theta }[/math], with

[math]\displaystyle{ \tan\theta = \frac{\sum_{k=0}^{K-1}\sin\omega t_k}{\sum_{k=0}^{K-1}\cos\omega t_k}, }[/math]

the probability density of amplitudes is given by

[math]\displaystyle{ \phi (A) = \frac{KA\cdot\operatorname{sock}}{2\lt x^2\gt }\exp\left(-\frac{KA^2}{4\lt x^2\gt }\cdot\operatorname{sock}\right), }[/math]

where the sock function is defined by

[math]\displaystyle{ \operatorname{sock}(\omega ,\theta) = \left[\frac{\cos^2\left(\theta - \theta_0\right)}{\alpha_0^2}+\frac{\sin^2\left(\theta - \theta_0\right)}{\beta_0^2}\right] }[/math]

and [math]\displaystyle{ \lt x^2\gt }[/math] denotes the variance of the dependent variable [math]\displaystyle{ x_k }[/math].

False-alarm probability and spectral significance

Integration of the pdf yields the false-alarm probability that white noise in the time domain produces an amplitude of at least [math]\displaystyle{ A }[/math],

[math]\displaystyle{ \Phi_\operatorname{FA}(A) = \exp\left(-\frac{KA^2}{4\lt x^2\gt }\cdot\operatorname{sock}\right). }[/math]

The sig is defined as the negative logarithm of the false-alarm probability and evaluates to

[math]\displaystyle{ \operatorname{sig}(A) = \frac{KA^2\log e}{4\lt x^2\gt }\cdot\operatorname{sock}. }[/math]

It returns the number of random time series one would have to examine to obtain one amplitude exceeding [math]\displaystyle{ A }[/math] at the given frequency and phase.

Applications

SigSpec is primarily used in asteroseismology to identify variable stars and to classify stellar pulsation (see references below). The fact that this method incorporates the properties of the time-domain sampling appropriately makes it a valuable tool for typical astronomical measurements containing data gaps.

See also

• Spectral density estimation

References

• M. Breger; S. M. Rucinski; P. Reegen (2007). "The Pulsation of EE Camelopardalis". The Astronomical Journal 134 (5): 1994–1998. doi:10.1086/522795. Bibcode: 2007AJ....134.1994B. 
• M. Gruberbauer; K. Kolenberg; J. F. Rowe; D. Huber; J. M. Matthews; P. Reegen; R. Kuschnig; C. Cameron et al. (2007). "MOST photometry of the RRdLyrae variable AQLeo: two radial modes, 32 combination frequencies and beyond". Monthly Notices of the Royal Astronomical Society 379 (4): 1498–1506. doi:10.1111/j.1365-2966.2007.12042.x. Bibcode: 2007MNRAS.379.1498G. 
• M. Gruberbauer; H. Saio; D. Huber; T. Kallinger; W. W. Weiss; D. B. Guenther; R. Kuschnig; J. M. Matthews et al. (2008). "MOST photometry and modeling of the rapidly oscillating (roAp) star γ Equulei". Astronomy and Astrophysics 480 (1): 223–232. doi:10.1051/0004-6361:20078830. Bibcode: 2008A&A...480..223G. 
• D. B. Guenther; T. Kallinger; P. Reegen; W. W. Weiss; J. M. Matthews; R. Kuschnig; A. F. J. Moffat; S. M. Rucinski et al. (2007). "Searching for p-modes in η Bootis & Procyon using MOST satellite data". Communications in Asteroseismology 151: 5–25. doi:10.1553/cia151s5. Bibcode: 2007CoAst.151....5G. 
• D. B. Guenther; T. Kallinger; K. Zwintz; W. W. Weiss; J. Tanner (2007). "Seismology of Pre-Main-Sequence Stars in NGC 6530". The Astrophysical Journal 671 (1): 581–591. doi:10.1086/522880. Bibcode: 2007ApJ...671..581G. http://library2.smu.ca/bitstream/01/25949/1/Guenther_David_B_article_2007_a.pdf. 
• D. Huber; H. Saio; M. Gruberbauer; W. W. Weiss; J. F. Rowe; M. Hareter; T. Kallinger; P. Reegen et al. (2008). "MOST photometry of the roAp star 10 Aquilae". Astronomy and Astrophysics 483 (1): 239–248. doi:10.1051/0004-6361:20079220. Bibcode: 2008A&A...483..239H. 
• T. Kallinger; D. B. Guenther; J. M. Matthews; W. W. Weiss; D. Huber; R. Kuschnig; A. F. J. Moffat; S. M. Rucinski et al. (2008). "Nonradial p-modes in the G9.5 giant ε Ophiuchi? Pulsation model fits to MOST photometry". Astronomy and Astrophysics 478 (2): 497–505. doi:10.1051/0004-6361:20078171. Bibcode: 2008A&A...478..497K. 
• T. Kallinger; P. Reegen; W. W. Weiss (2008). "A heuristic derivation of the uncertainty for frequency determination in time series data". Astronomy and Astrophysics 481 (2): 571–574. doi:10.1051/0004-6361:20077559. Bibcode: 2008A&A...481..571K. 
• P. Reegen (2005). ""SigSpec - reliable computation of significance in Fourier space", in The A-Star Puzzle, Proceedings IAU Symp. 224, eds. J. Zverko, J. Ziznovsky, S.J. Adelman, W.W. Weiss". The A-Star Puzzle, Proceedings of IAU Symposium 224. Cambridge, UK: Cambridge University Press. pp. 791–798. ISBN 0-521-85018-5. 
• P. Reegen; M. Gruberbauer; L. Schneider; W. W. Weiss (2008). "Cinderella - Comparison of INDEpendent RELative Least-squares Amplitudes". Astronomy and Astrophysics 484 (2): 601–608. doi:10.1051/0004-6361:20078855. Bibcode: 2008A&A...484..601R. 
• C. Schoenaers; A. E. Lynas-Gray (2007). "A new slowly pulsating subdwarf-B star: HD 4539". Communications in Asteroseismology 151: 67–76. doi:10.1553/cia151s67. Bibcode: 2007CoAst.151...67S. 
• M. Zechmeister; M. Kuerster (2009). "The gemeralised Lomb-Scargle periodogram. A new formalism for the floating-mean and Keplerian periodograms". Astronomy and Astrophysics 496 (2): 577–584. doi:10.1051/0004-6361:200811296. Bibcode: 2009A&A...496..577Z. 
• K. Zwintz; T. Kallinger; D. B. Guenther; M. Gruberbauer; D. Huber; J. Rowe; R. Kuschnig; W. W. Weiss et al. (2009). "MOST photometry of the enigmatic PMS pulsator HD 142666". Astronomy and Astrophysics 494 (3): 1031–1040. doi:10.1051/0004-6361:200811116. Bibcode: 2009A&A...494.1031Z. 
• K. Zwintz; M. Hareter; R. Kuschnig; P. J. Amado; N. Nesvacil; E. Rodriguez; D. Diaz-Fraile; W. W. Weiss et al. (2009). "MOST observations of the young open cluster NGC 2264". Astronomy and Astrophysics 502: 1239–252. doi:10.1051/0004-6361/200911863. 

External links

• Website with further information on SigSpec calculation, etc.