000510194 001__ 510194
000510194 003__ SzGeCERN
000510194 005__ 20220422103920.0
000510194 0247_ $$2DOI$$a10.1086/375264
000510194 0248_ $$aoai:cds.cern.ch:510194$$pcerncds:FULLTEXT$$pcerncds:CERN:FULLTEXT$$pcerncds:CERN
000510194 035__ $$a2265820CERCER
000510194 035__ $$9SPIRES$$a4801890
000510194 035__ $$9Inspire$$a567992
000510194 037__ $$9arXiv$$aastro-ph/0107419$$castro-ph
000510194 037__ $$aFERMILAB-PUB-01-270-A
000510194 041__ $$aeng
000510194 088__ $$aFERMILAB-PUB-2001-270-A
000510194 100__ $$aSzalay, Alexander S.$$uJohns Hopkins U.
000510194 245__ $$aKL Estimation of the Power Spectrum Parameters from the Angular Distribution of Galaxies in Early SDSS Data
000510194 246__ $$aSLOAN DIGITAL SKY SURVEY
000510194 260__ $$c2002
000510194 269__ $$aBatavia, IL$$bFERMILAB$$c20 Jul 2001
000510194 300__ $$a25 p
000510194 520__ $$aWe present measurements of parameters of the 3-dimensional power spectrum of galaxy clustering from 222 square degrees of early imaging data in the Sloan Digital Sky Survey. The projected galaxy distribution on the sky is expanded over a set of Karhunen-Loeve eigenfunctions, which optimize the signal-to-noise ratio in our analysis. A maximum likelihood analysis is used to estimate parameters that set the shape and amplitude of the 3-dimensional power spectrum. Our best estimates are Gamma=0.188 +/- 0.04 and sigma_8L = 0.915 +/- 0.06 (statistical errors only), for a flat Universe with a cosmological constant. We demonstrate that our measurements contain signal from scales at or beyond the peak of the 3D power spectrum. We discuss how the results scale with systematic uncertainties, like the radial selection function. We find that the central values satisfy the analytically estimated scaling relation. We have also explored the effects of evolutionary corrections, various truncations of the KL basis, seeing, sample size and limiting magnitude. We find that the impact of most of these uncertainties stay within the 2-sigma uncertainties of our fiducial result.
000510194 520__ $$9IOP$$aWe present measurements of parameters of the three-dimensional power spectrum of galaxy clustering from 222 square degrees of early imaging data in the Sloan Digital Sky Survey (SDSS). The projected galaxy distribution on the sky is expanded over a set of Karhunen-Lo?ve (KL) eigenfunctions, which optimize the signal-to-noise ratio in our analysis. A maximum likelihood analysis is used to estimate parameters that set the shape and amplitude of the three-dimensional power spectrum of galaxies in the SDSS magnitude-limited sample withr* < 21. Our best estimates are ? = 0.188 ? 0.04 and ?8L= 0.915 ? 0.06 (statistical errors only), for a flat universe with a cosmological constant. We demonstrate that our measurements contain signal from scales at or beyond the peak of the three-dimensional power spectrum. We discuss how the results scale with systematic uncertainties, like the radial selection function. We find that the central values satisfy the analytically estimated scaling relation. We have also explored the effects of evolutionary corrections, various truncations of the KL basis, seeing, sample size, and limiting magnitude. We find that the impact of most of these uncertainties stay within the 2 ? uncertainties of our fiducial result.
000510194 595__ $$aLANL EDS
000510194 595__ $$aSIS ING2004
000510194 595__ $$aSIS:2004 PR/LKR added
000510194 65017 $$2SzGeCERN$$aAstrophysics and Astronomy
000510194 695__ $$9LANL EDS$$aAstrophysics
000510194 690C_ $$aARTICLE
000510194 690C_ $$aCERN
000510194 700__ $$aJain, Bhuvnesh$$uPennsylvania U.$$uJohns Hopkins U.
000510194 700__ $$aMatsubara, Takahiko$$uNagoya U.
000510194 700__ $$aScranton, Ryan$$uFermilab$$uChicago U., Astron. Astrophys. Ctr.
000510194 700__ $$aVogeley, Michael S.$$uDrexel U.
000510194 700__ $$aConnolly, Andrew$$uPittsburgh U.
000510194 700__ $$aDodelson, Scott$$iINSPIRE-00077513$$uFermilab$$uChicago U., Astron. Astrophys. Ctr.
000510194 700__ $$aEisenstein, Daniel$$uArizona U., Astron. Dept. - Steward Observ.
000510194 700__ $$aFrieman, Joshua A.$$uFermilab$$uChicago U., Astron. Astrophys. Ctr.
000510194 700__ $$aGunn, James E.$$uPrinceton U. Observ.
000510194 700__ $$aHui, Lam$$uColumbia U.
000510194 700__ $$aJohnston, David$$uFermilab$$uChicago U., Astron. Astrophys. Ctr.
000510194 700__ $$aKent, Stephen M.$$uFermilab
000510194 700__ $$aKerscher, Martin$$uJohns Hopkins U.
000510194 700__ $$aLoveday, Jon$$uSussex U., Astron. Ctr.
000510194 700__ $$aMeiksin, Avery$$uEdinburgh U., Inst. Astron.
000510194 700__ $$aNarayanan, Vijay$$uPrinceton U. Observ.
000510194 700__ $$aNichol, Robert C.$$uCarnegie Mellon U.
000510194 700__ $$aO'Connell, Liam$$uSussex U., Astron. Ctr.
000510194 700__ $$aPope, Adrian$$uJohns Hopkins U.
000510194 700__ $$aScoccimarro, Roman$$uNew York U.$$uPrinceton, Inst. Advanced Study
000510194 700__ $$aSheth, Ravi K.$$uFermilab
000510194 700__ $$aStebbins, Albert$$uFermilab
000510194 700__ $$aStrauss, Michael A.$$uPrinceton U. Observ.
000510194 700__ $$aSzapudi, Istvan$$uInst. Astron., Honolulu
000510194 700__ $$aTegmark, Max$$iINSPIRE-00130936$$uPennsylvania U.
000510194 700__ $$aZehavi, Idit$$uFermilab
000510194 700__ $$aAnnis, James$$uFermilab
000510194 700__ $$aBahcall, Neta A.$$uPrinceton U. Observ.
000510194 700__ $$aBrinkmann, Jon$$uApache Point Observ.
000510194 700__ $$aCsabai, Istvan$$uEotvos U.
000510194 700__ $$aFukugita, Masataka$$uTokyo U., ICRR
000510194 700__ $$aHennessy, Greg$$uNaval Observ., Wash., D.C.
000510194 700__ $$aHogg, David W.$$uNew York U.
000510194 700__ $$aIvezic, Zeljko$$uPrinceton U. Observ.
000510194 700__ $$aKnapp, Gillian R.$$uPrinceton U. Observ.
000510194 700__ $$aKunszt, Peter Z.$$uCERN
000510194 700__ $$aLamb, Don Q.$$uChicago U., Astron. Astrophys. Ctr.
000510194 700__ $$aLee, Brian C.$$uFermilab
000510194 700__ $$aLupton, Robert H.$$uPrinceton U. Observ.
000510194 700__ $$aMunn, Jeffrey R.$$uNaval Observ., Flagstaff
000510194 700__ $$aPeoples, John$$uFermilab
000510194 700__ $$aPier, Jeffrey R.$$uNaval Observ., Flagstaff
000510194 700__ $$aRockosi, Constance$$uChicago U., Astron. Astrophys. Ctr.
000510194 700__ $$aSchlegel, David$$uPrinceton U. Observ.
000510194 700__ $$aStoughton, Christopher$$uFermilab
000510194 700__ $$aTucker, Douglas L.$$uFermilab
000510194 700__ $$aYanny, Brian$$uFermilab
000510194 700__ $$aYork, Donald G.$$uChicago U., Astron. Astrophys. Ctr.
000510194 710__ $$gSDSS Collaboration
000510194 720__ $$aSzalay, Alexander S.
000510194 720__ $$aJain, Bhuvnesh
000510194 720__ $$aMatsubara, Takahiko
000510194 720__ $$aScranton, Ryan
000510194 720__ $$aVogeley, Michael S.
000510194 720__ $$aConnolly, Andrew
000510194 720__ $$aDodelson, Scott
000510194 720__ $$aEisenstein, Daniel
000510194 720__ $$aFrieman, Joshua A.
000510194 720__ $$aGunn, James E.
000510194 720__ $$aHui, Lam
000510194 720__ $$aJohnston, David
000510194 720__ $$aKent, Stephen
000510194 720__ $$aKerscher, Martin
000510194 720__ $$aLoveday, Jon
000510194 720__ $$aMeiksin, Avery
000510194 720__ $$aNarayanan, Vijay
000510194 720__ $$aNichol, Robert C.
000510194 720__ $$aConnell, Liam O'
000510194 720__ $$aPope, Adrian
000510194 720__ $$aScoccimarro, Roman
000510194 720__ $$aSheth, Ravi K.
000510194 720__ $$aStebbins, Albert
000510194 720__ $$aStrauss, Michael A.
000510194 720__ $$aSzapudi, Istvan
000510194 720__ $$aTegmark, Max
000510194 720__ $$aZehavi, Idit
000510194 773__ $$c191-205$$n1$$pAstrophys. J.$$v571$$y2002
000510194 859__ $$fmax@hep.upenn.edu
000510194 8564_ $$uhttp://lss.fnal.gov/archive/2001/pub/Pub-01-270-A.pdf$$yFermilab Library Server (fulltext available)
000510194 8564_ $$81303255$$s939704$$uhttp://cds.cern.ch/record/510194/files/arXiv:astro-ph_0107419.pdf
000510194 8564_ $$81502582$$s966216$$uhttp://cds.cern.ch/record/510194/files/Pub-01-270-A.pdf$$yFulltext
000510194 8564_ $$8401911$$s1484114$$uhttp://cds.cern.ch/record/510194/files/0107419.pdf$$yAccess to fulltext document
000510194 8564_ $$8401911$$s387149$$uhttp://cds.cern.ch/record/510194/files/0107419.ps.gz$$yAccess to fulltext document
000510194 916__ $$sn$$w200130
000510194 960__ $$a13
000510194 961__ $$c20100420$$h1349$$lCER01$$x20010723
000510194 963__ $$aPUBLIC
000510194 970__ $$a002265820CER
000510194 980__ $$aARTICLE