Препринт

The Atacama Cosmology Telescope: Large-scale velocity reconstruction with the kinematic Sunyaev--Zel'dovich effect and DESI LRGs

Fiona McCarthyNicholas BattagliaDepartment of Astronomy , Cornell University , Ithaca , NY , USA 14850Rachel BeanDepartment of Astronomy , Cornell University , Ithaca , NY , USA 14850J. Richard BondCanadian Institute for Theoretical Astrophysics , 60 St. George Street ,Hongbo CaiDepartment of Physics and Astronomy , University of Pittsburgh , Pittsburgh , PA , USA 15260Erminia CalabreseSchool of Physics and Astronomy , Cardiff University , The Parade , Cardiff , Wales CF24 3AA , UKWilliam R. CoultonDAMTP , Centre for Mathematical Sciences , Wilberforce Road , Cambridge CB3 0WA , UKMark J. DevlinDepartment of Physics and Astronomy , University of Pennsylvania , 209 South 33rd Street , Philadelphia , PA , USA 19104Jo DunkleyS. FerraroPhysics Division , Lawrence Berkeley National Laboratory , Berkeley , CA , USAVera GluscevicDepartment of Physics and Astronomy , University of Southern California , Los Angeles , CA , 90007 , USAYilun GuanDunlap Institute for Astronomy & Astrophysics , University of Toronto , 50 St. George St. , Toronto ON M5S 3H4 , CanadaJ. Colin HillDepartment of Physics , Columbia University , New York , NY , USA 10027Matthew C. JohnsonDepartment of Physics and Astronomy , York University , Toronto , ON M3J 1P3 , CanadaAleksandra KusiakKavli Institute for Cosmology Cambridge , Madingley Road , Cambridge , CB3 0HA , UKAlex LaguëN. MacCrannDAMTP , Centre for Mathematical Sciences , Wilberforce Road , Cambridge CB3 0WA , UKMathew S. MadhavacherilDepartment of Physics and Astronomy , University of Pennsylvania , 209 South 33rd Street , Philadelphia , PA , USA 19104Kavilan MoodleyAstrophysics Research Centre , University of KwaZulu-Natal , Westville Campus , Durban 4041 , South AfricaSigurd NæssInstitute for theoretical astrophysics , University of Oslo , NorwayFrank J. QuBernardita Ried GuachallaDepartment of Physics , Stanford University , Stanford , CA , USA 94305-4085 25Neelima SehgalPhysics and Astronomy Department , Stony Brook University , Stony Brook , NY 11794 , USABlake D. SherwinDAMTP , Centre for Mathematical Sciences , Wilberforce Road , Cambridge CB3 0WA , UKCristobál SifónKendrick M. SmithPerimeter Institute for Theoretical Physics , 31 Caroline St N , Waterloo , ON N2L 2Y5 , CanadaSuzanne T. StaggsJoseph Henry Laboratories of Physics , Jadwin Hall , Princeton University , Princeton , NJ , USA 08544Alexander van EngelenSchool of Earth and Space Exploration , Arizona State University , Tempe , AZ 85287 , USAEve M. VavagiakisDepartment of Astronomy , Cornell University , Ithaca , NY , USA 14850Edward J. WollackNASA Goddard Space Flight Center , Greenbelt , MD USA 20771

2024en

ABI

Аннотация

The kinematic Sunyaev--Zel'dovich (kSZ) effect induces a non-zero density-density-temperature bispectrum, which we can use to reconstruct the large-scale velocity field from a combination of cosmic microwave background (CMB) and galaxy density measurements, in a procedure known as ``kSZ velocity reconstruction''. This method has been forecast to constrain large-scale modes with future galaxy and CMB surveys, improving their measurement beyond what is possible with the galaxy surveys alone. Such measurements will enable tighter constraints on large-scale signals such as primordial non-Gaussianity, deviations from homogeneity, and modified gravity. In this work, we demonstrate a statistically significant measurement of kSZ velocity reconstruction for the first time, by applying quadratic estimators to the combination of the ACT DR6 CMB+kSZ map and the DESI LRG galaxies (with photometric redshifts) in order to reconstruct the velocity field. We do so using a formalism appropriate for the 2-dimensional projected galaxy fields that we use, which naturally incorporates the curved-sky effects important on the largest scales. We find evidence for the signal by cross-correlating with an external estimate of the velocity field from the spectroscopic BOSS survey and rejecting the null (no-kSZ) hypothesis at $3.8σ$. Our work presents a first step towards the use of this observable for cosmological analyses.

Ҳали таржима қилинмаган

Идентификаторлар

DOI: 10.48550/arxiv.2410.06229

Иқтибослар ва манбалар

0 та иқтибос0 та фойдаланилган манба