Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.sao.ru/cats/~satr/RFSymp/abs/38_Verkhodanov2.ps Дата изменения: Mon Oct 9 13:07:34 2006 Дата индексирования: Tue Oct 2 10:49:46 2012 Кодировка: Поисковые слова: http astrokuban.info astrokuban

PHASE ANALYSIS IN STUDY OF COSMIC MICROWAVE
BACKGROUND
O.V.Verkhodanov 1 , P.D.Naselsky 2 , L.­Y.Chiang 2 , A.G.Doroshkevich 3 , I.D.Novikov 3,2
1 Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, Russia
2 Niels Bohr Institute, Copenhagen, Denmark
3 AstroSpace Center, Moscow, Russia
vo@sao.ru
Phase analysis based on the complex values of spherical harmonics of the CMB fluctuation
expansion is an extremely important method of observational cosmology. We consider
several aspects of phase analysis in the CMB study. They concern the problems of signal
restoration (Naselsky et al. 2005), search for non­Gaussianity (Chiang et al. 2003) and
study of the foreground contamination of this separated CMB signal (Naseslky et al. 2003,
2004, 2005). Using the GLESP (Gauss­LEgendre Sky Pixelization) package (Doroshkevich
et al. 2005) for CMB analysis we produce phase data for spherical harmonics in the form
of a #m = |# #m | exp(i# #m ), where a #m ­s are coe#cients of spherical harmonics of the #--
multipole in the m--mode, |# #m | is their amplitude, # #m is a phase, and i is the imaginary
unit. Considering the minimum in correlation of phases of CMB and foregrounds we can
separate the signal corresponding to these properties at low # (# # 100) where the point
source influence is minimal. Another important moment is the study of the Gaussianity
problem in the CMB observational data. To check statistical properties of the data we
produce phase diagrams. These diagrams demonstrate the strong non­Gaussianity for all
accessible maps of CMB. The high phase correlations between CMB and foregrounds hint
us about problems of signal separation. Similar approaches are developed for the Planck
mission.
Acknowledgements. This work is supported particularly by the Russian Foundation of
Basic Research (grants No 05­07­90139 and 05­02­16302).
References
Chiang L.­Y., Naselsky P.D., Verkhodanov O.V., Way M.J.'' Astrophys. J., 2003, 590, L65
(astro­ph/0303643)
Naselsky P.D., Doroshkevich A.G. , Verkhodanov O.V.: Astrophys. J., 2003, 599, L53
(astro­ph/0310542)
Naselsky P.D., Doroshkevich A.G., Verkhodanov O.V.: MNRAS, 2004, 349, 695 (astro­
ph/0310601)
Naselsky P.D., Chiang L.­Y., Novikov I.D., Verkhodanov O.V.: Internat. J. Mod. Phys.
D, 2005, 14, 1273 (astro­ph/0405523)
Doroshkevich A.G., Naselsky P.D., Verkhodanov O.V., Novikov D.I., Turchaninov V.I.,
Novikov I.D., Christensen P.R., Chiang L.­Y.: Internat. J. Mod. Phys. D, 2005, 14, 275
(astro­ph/0305537)