002783167 001__ 2783167
002783167 005__ 20230322160150.0
002783167 0248_ $$aoai:cds.cern.ch:2783167$$pcerncds:FULLTEXT$$pcerncds:CERN:FULLTEXT$$pcerncds:CERN
002783167 0247_ $$2DOI$$9APS$$a10.1103/PhysRevD.105.043531$$qpublication
002783167 037__ $$9arXiv$$aarXiv:2110.00006$$castro-ph.CO
002783167 037__ $$9arXiv:reportnumber$$aYITP-21-106
002783167 037__ $$9arXiv:reportnumber$$aYITP-21-10
002783167 037__ $$9arXiv:reportnumber$$aCERN-TH-2021-143
002783167 035__ $$9arXiv$$aoai:arXiv.org:2110.00006
002783167 035__ $$9Inspire$$aoai:inspirehep.net:1937373$$d2021-10-27T16:25:41Z$$h2021-10-29T02:02:51Z$$mmarcxml$$ttrue$$uhttps://inspirehep.net/api/oai2d
002783167 035__ $$9Inspire$$a1937373
002783167 041__ $$aeng
002783167 100__ $$aIvanov, Mikhail [email protected]$$uPrinceton, Inst. Advanced Study$$vSchool of Natural Sciences, Institute for Advanced Study, 1 Einstein Drive, Princeton, New Jersey 08540, USA$$vSchool of Natural Sciences, Institute for Advanced Study, 1 Einstein Drive, Princeton, NJ 08540, USA$$vEinstein Fellow
002783167 245__ $$9APS$$aCosmological constraints without nonlinear redshift-space distortions
002783167 246__ $$9arXiv$$aCosmological constraints without fingers of God
002783167 269__ $$c2021-09-30
002783167 260__ $$c2022-02-15
002783167 300__ $$a17 p
002783167 500__ $$9arXiv$$a29 pages, 6 figures, minor edits, new BOSS likelihood used, available
at github.com/oliverphilcox/full_shape_likelihoods
002783167 520__ $$9APS$$aNonlinear redshift-space distortions (“fingers of God”) are challenging to model analytically, a fact that limits the applicability of perturbation theory (PT) in redshift space as compared to real space. We show how this problem can be mitigated using a new observable, <math display="inline"><msub><mi>Q</mi><mn>0</mn></msub></math>, which can be easily estimated from the redshift-space clustering data and is approximately equal to the real-space power spectrum. The new statistic does not suffer from fingers of God and can be accurately described with PT down to <math display="inline"><mrow><msub><mrow><mi>k</mi></mrow><mrow><mi>max</mi></mrow></msub><mo>≃</mo><mn>0.4</mn><mtext> </mtext><mtext> </mtext><mi>h</mi><mtext> </mtext><msup><mrow><mi>Mpc</mi></mrow><mrow><mo>-</mo><mn>1</mn></mrow></msup></mrow></math>. It can be straightforwardly included in the likelihood at negligible additional computational cost and yields noticeable improvements on cosmological parameters compared to standard power spectrum multipole analyses. Using both simulations and observational data from the Baryon Oscillation Spectroscopic Survey, we show that improvements vary from 10% to 100% depending on the cosmological parameter considered, the galaxy sample, and the survey volume.
002783167 520__ $$9arXiv$$aNon-linear redshift-space distortions ("fingers of God") are challenging to model analytically, a fact that limits the applicability of perturbation theory in redshift space as compared to real space. We show how this problem can be mitigated using a new observable, $Q_0$, which can be easily estimated from the redshift space clustering data and is approximately equal to the real space power spectrum. The new statistic does not suffer from fingers of God and can be accurately described with perturbation theory down to $k_{\rm max}\simeq 0.4~h~\text{Mpc}^{-1}$. It can be straightforwardly included in the likelihood at negligible additional computational cost, and yields noticeable improvements on cosmological parameters compared to standard power spectrum multipole analyses. Using both simulations and observational data from the Baryon Oscillation Spectroscopic Survey, we show that improvements vary from $10\%$ to $100\%$ depending on the cosmological parameter considered, the galaxy sample and the survey volume.
002783167 540__ $$3preprint$$aarXiv nonexclusive-distrib 1.0$$uhttp://arxiv.org/licenses/nonexclusive-distrib/1.0/
002783167 540__ $$3publication$$aCC BY 4.0$$fCERN-RP : APS$$uhttps://creativecommons.org/licenses/by/4.0/
002783167 542__ $$3publication$$dauthors$$g2022
002783167 595__ $$aCERN-TH
002783167 595_D $$aZ$$d2021-10-06$$sabs
002783167 595_D $$aZ$$d2021-10-12$$sprinted
002783167 65017 $$2arXiv$$aastro-ph.CO
002783167 65017 $$2SzGeCERN$$aAstrophysics and Astronomy
002783167 690C_ $$aCERN
002783167 690C_ $$aARTICLE
002783167 700__ $$aPhilcox, Oliver H.E.$$uPrinceton, Inst. Advanced Study$$uPrinceton U., Astrophys. Sci. Dept.$$uCambridge U., DAMTP$$vSchool of Natural Sciences, Institute for Advanced Study, 1 Einstein Drive, Princeton, New Jersey 08540, USA$$vDepartment of Applied Mathematics and Theoretical Physics, University of Cambridge, Cambridge CB3 0WA, United Kingdom$$vDepartment of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08540, USA$$vSchool of Natural Sciences, Institute for Advanced Study, 1 Einstein Drive, Princeton, NJ 08540, USA$$vDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08540, USA$$vDepartment of Applied Mathematics and Theoretical Physics, University of Cambridge, Cambridge CB3 0WA, UK
002783167 700__ $$aSimonović, Marko$$uCERN$$vTheoretical Physics Department, CERN, 1 Esplanade des Particules, Geneva 23, CH-1211, Switzerland$$vTheoretical Physics Department, CERN, 1 Esplanade des Particules, Geneva 23, CH-1211, Switzerland
002783167 700__ $$aZaldarriaga, Matias$$uPrinceton, Inst. Advanced Study$$vSchool of Natural Sciences, Institute for Advanced Study, 1 Einstein Drive, Princeton, New Jersey 08540, USA$$vSchool of Natural Sciences, Institute for Advanced Study, 1 Einstein Drive, Princeton, NJ 08540, USA
002783167 700__ $$aNischimichi, Takahiro$$uKyoto U., Yukawa Inst., Kyoto$$uTokyo U., IPMU$$vCenter for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan$$vKavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS The University of Tokyo, Kashiwa, Chiba 277-8583, Japan$$vCenter for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan$$vKavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
002783167 700__ $$aTakada, Masahiro$$uTokyo U., IPMU$$vKavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS The University of Tokyo, Kashiwa, Chiba 277-8583, Japan$$vKavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
002783167 773__ $$c043531$$mpublication$$n4$$pPhys. Rev. D$$v105$$xPhys. Rev. D 105, 043531 (2022)$$y2022
002783167 8564_ $$82325693$$s270983$$uhttp://cds.cern.ch/record/2783167/files/mu0_marg.png$$y00004 Posteriors from the PT challenge data for the analysis with fixed $\Omega_b/\Omega_m$ and $n_s$.
002783167 8564_ $$82325694$$s8686$$uhttp://cds.cern.ch/record/2783167/files/Pls.png$$y00001 \textbf{Upper panel}: Comparison of moments, $Q_n$, and multipoles, $P_\ell$, for the redshift-space power spectrum of PT challenge galaxies. The real space power spectrum $P_{\rm gg}$ (rescaled to match the AP effect present in $Q_0$) in the left plot is slightly shifted horizontally for clarity, as the datapoints overlap with those of $Q_0$. \textbf{Lower panel}: Higher-order Legendre multipoles with $\ell=4,6,8$.
002783167 8564_ $$82325695$$s17926$$uhttp://cds.cern.ch/record/2783167/files/Qns.png$$y00000 \textbf{Upper panel}: Comparison of moments, $Q_n$, and multipoles, $P_\ell$, for the redshift-space power spectrum of PT challenge galaxies. The real space power spectrum $P_{\rm gg}$ (rescaled to match the AP effect present in $Q_0$) in the left plot is slightly shifted horizontally for clarity, as the datapoints overlap with those of $Q_0$. \textbf{Lower panel}: Higher-order Legendre multipoles with $\ell=4,6,8$.
002783167 8564_ $$82325696$$s337144$$uhttp://cds.cern.ch/record/2783167/files/mu0_bbnlike_final.png$$y00005 Posteriors from the analysis of the PT challenge mock galaxy power spectrum with a prior on $\omega_b$.
002783167 8564_ $$82325697$$s114935$$uhttp://cds.cern.ch/record/2783167/files/OR_Q0.png$$y00007 Posteriors from the cosmological analysis of the Outer Rim emission line galaxy mock power spectrum measurements.
002783167 8564_ $$82325698$$s3436275$$uhttp://cds.cern.ch/record/2783167/files/2110.00006.pdf$$yFulltext
002783167 8564_ $$82325699$$s153147$$uhttp://cds.cern.ch/record/2783167/files/boss_q0.png$$y00006 Posteriors from the cosmological analysis of the BOSS galaxy power spectrum measurements combined with the BBN prior on $\omega_b$.
002783167 8564_ $$82325700$$s19960$$uhttp://cds.cern.ch/record/2783167/files/Plhigh.png$$y00002 \textbf{Upper panel}: Comparison of moments, $Q_n$, and multipoles, $P_\ell$, for the redshift-space power spectrum of PT challenge galaxies. The real space power spectrum $P_{\rm gg}$ (rescaled to match the AP effect present in $Q_0$) in the left plot is slightly shifted horizontally for clarity, as the datapoints overlap with those of $Q_0$. \textbf{Lower panel}: Higher-order Legendre multipoles with $\ell=4,6,8$.
002783167 8564_ $$82325701$$s21590$$uhttp://cds.cern.ch/record/2783167/files/higher.png$$y00003 Higher order multipoles of the PT challenge data and their fits by quadratic polynomials.
002783167 8564_ $$82352590$$s8686$$uhttp://cds.cern.ch/record/2783167/files/w1_Pls.png$$y00001 \textbf{Upper panel}: Comparison of moments, $Q_n$, and multipoles, $P_\ell$, for the redshift-space power spectrum of PT challenge galaxies. The real space power spectrum $P_{\rm gg}$ (rescaled to match the AP effect present in $Q_0$) in the left plot is slightly shifted horizontally for clarity, as the datapoints overlap with those of $Q_0$. \textbf{Lower panel}: Higher-order Legendre multipoles with $\ell=4,6,8$.
002783167 8564_ $$82352591$$s17926$$uhttp://cds.cern.ch/record/2783167/files/w0_Qns.png$$y00000 \textbf{Upper panel}: Comparison of moments, $Q_n$, and multipoles, $P_\ell$, for the redshift-space power spectrum of PT challenge galaxies. The real space power spectrum $P_{\rm gg}$ (rescaled to match the AP effect present in $Q_0$) in the left plot is slightly shifted horizontally for clarity, as the datapoints overlap with those of $Q_0$. \textbf{Lower panel}: Higher-order Legendre multipoles with $\ell=4,6,8$.
002783167 8564_ $$82352592$$s270983$$uhttp://cds.cern.ch/record/2783167/files/w4_mu0_marg.png$$y00004 Posteriors from the PT challenge data for the analysis with fixed $\Omega_b/\Omega_m$ and $n_s$.
002783167 8564_ $$82352593$$s19960$$uhttp://cds.cern.ch/record/2783167/files/w2_Plhigh.png$$y00002 \textbf{Upper panel}: Comparison of moments, $Q_n$, and multipoles, $P_\ell$, for the redshift-space power spectrum of PT challenge galaxies. The real space power spectrum $P_{\rm gg}$ (rescaled to match the AP effect present in $Q_0$) in the left plot is slightly shifted horizontally for clarity, as the datapoints overlap with those of $Q_0$. \textbf{Lower panel}: Higher-order Legendre multipoles with $\ell=4,6,8$.
002783167 8564_ $$82352594$$s121496$$uhttp://cds.cern.ch/record/2783167/files/w7_OR_Q0.png$$y00007 Posteriors from the cosmological analysis of the Outer Rim (OR) emission line galaxy mock power spectrum measurements.
002783167 8564_ $$82352595$$s21590$$uhttp://cds.cern.ch/record/2783167/files/w3_higher.png$$y00003 Higher order multipoles of the PT challenge data and their fits by quadratic polynomials.
002783167 8564_ $$82352596$$s337144$$uhttp://cds.cern.ch/record/2783167/files/w5_mu0_bbnlike_final.png$$y00005 Posteriors from the analysis of the PT challenge mock galaxy power spectrum with a prior on $\omega_b$.
002783167 8564_ $$82352597$$s146393$$uhttp://cds.cern.ch/record/2783167/files/w6_boss_q0.png$$y00006 Posteriors from the cosmological analysis of the BOSS galaxy power spectrum measurements combined with the BBN prior on $\omega_b$.
002783167 8564_ $$82352746$$s1639832$$uhttp://cds.cern.ch/record/2783167/files/PhysRevD.105.043531.pdf$$yFulltext
002783167 8564_ $$82352746$$s12734$$uhttp://cds.cern.ch/record/2783167/files/PhysRevD.105.043531.gif?subformat=icon$$xicon$$yFulltext
002783167 8564_ $$82352746$$s187948$$uhttp://cds.cern.ch/record/2783167/files/PhysRevD.105.043531.jpg?subformat=icon-700$$xicon-700$$yFulltext
002783167 8564_ $$82352746$$s34394$$uhttp://cds.cern.ch/record/2783167/files/PhysRevD.105.043531.jpg?subformat=icon-180$$xicon-180$$yFulltext
002783167 960__ $$a13
002783167 980__ $$aARTICLE