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Constraining primordial non-Gaussianity from DESI quasar targets and Planck CMB lensing

Alex KrolewskiPerimeter Institute for Theoretical Physics, 31 Caroline St. North, Waterloo, ON NL2 2Y5, CanadaWill J. PercivalDepartment of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1, CanadaS. FerraroDepartment of Physics, University of California, Berkeley, Berkeley, CA 94720, U.S.AE. ChaussidonIRFU, CEA, Université Paris-Saclay, Gif-sur-Yvette F-91191, FranceMehdi RezaieDepartment of Physics, Kansas State University, 116 Cardwell Hall, Manhattan, KS 66506, U.S.AJ. AguilarPhysics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, U.S.AS. AhlenPhysics Department, Boston University, 590 Commonwealth Avenue, Boston, MA 02215, U.S.ADavid BrooksDepartment of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, U.KKyle DawsonDepartment of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, U.S.AAxel de la MacorraInstituto de Física, Universidad Nacional Autónoma de México, Cd. de México C.P. 04510, MéxicoP. DoelDepartment of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, U.KK. FanningCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, U.S.AAndreu Font-RiberaInstitut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, Bellaterra 08193, Barcelona, SpainSatya Gontcho A GontchoPhysics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, U.S.AJ. GuyPhysics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, U.S.AK. HonscheidCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, U.S.AR. KehoeDepartment of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75275, U.S.ATheodore KisnerPhysics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, U.S.AAnthony KreminPhysics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, U.S.AMartin LandriauPhysics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, U.S.AM. E. LeviPhysics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, U.S.APaul MartiniCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, U.S.AAaron MeisnerNSF's NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AR. MiquelCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, U.S.AJundan NieNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing 100012, P.R. ChinaClaire PoppettPhysics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, U.S.AA.J. RossCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, U.S.AGraziano RossiDepartment of Physics and Astronomy, Sejong University, Seoul 143-747, KoreaM. SchubnellUniversity of Michigan, Ann Arbor, MI 48109, U.S.AHee‐Jong SeoDepartment of Physics and Astronomy, Ohio University, Athens, OH 45701, U.S.AG. TarléUniversity of Michigan, Ann Arbor, MI 48109, U.S.AM. Vargas-MagañaInstituto de Física, Universidad Nacional Autónoma de México, Cd. de México C.P. 04510, MéxicoBenjamin A. WeaverNSF's NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, U.S.AChristophe YècheIRFU, CEA, Université Paris-Saclay, Gif-sur-Yvette F-91191, FranceRongpu ZhouPhysics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, U.S.AZhimin ZhouNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing 100012, P.R. China

2024en

ABI

Annotatsiya

Abstract We detect the cross-correlation between 2.7 million DESI quasar targets across 14,700 deg 2 (180 quasars deg -2 ) and Planck 2018 CMB lensing at ∼30 σ . We use the cross-correlation on very large scales to constrain local primordial non-Gaussianity via the scale dependence of quasar bias. The DESI quasar targets lie at an effective redshift of 1.51 and are separated into four imaging regions of varying depth and image quality. We select quasar targets from Legacy Survey DR9 imaging, apply additional flux and photometric redshift cuts to improve the purity and reduce the fraction of unclassified redshifts, and use early DESI spectroscopy of 194,000 quasar targets to determine their redshift distribution and stellar contamination fraction (2.6%). Due to significant excess large-scale power in the quasar autocorrelation, we apply weights to mitigate contamination from imaging systematics such as depth, extinction, and stellar density. We use realistic contaminated mocks to determine the greatest number of systematic modes that we can fit, before we are biased by overfitting and spuriously remove real power. We find that linear regression with one to seven imaging templates removed per region accurately recovers the input cross-power, f NL and linear bias. As in previous analyses, our f NL constraint depends on the linear primordial non-Gaussianity bias parameter, b ϕ = 2( b - p ) δ c assuming universality of the halo mass function. We measure f NL = -26 +45 -40 with p = 1.6 ( f NL = -18 +29 -27 with p = 1.0), and find that this result is robust under several systematics tests. Future spectroscopic quasar cross-correlations with Planck lensing can tighten the f NL constraints by a factor of 2 if they can remove the excess power on large scales in the quasar auto power spectrum.

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DOI: 10.1088/1475-7516/2024/03/021

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