Probing cosmic velocities with the pairwise kinematic Sunyaev-Zel’dovich signal in DESI Bright Galaxy Sample DR1 and ACT DR6

We present a measurement of the pairwise kinematic Sunyaev-Zel’dovich (kSZ) signal using the Dark Energy Spectroscopic Instrument (DESI) Bright Galaxy Sample (BGS) Data Release 1 (DR1) galaxy sample overlapping with the Atacama Cosmology Telescope (ACT) CMB temperature map. Our analysis makes use of 1.6 million galaxies with stellar masses <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"> <a:mi>log</a:mi> <a:msub> <a:mi>M</a:mi> <a:mo>⋆</a:mo> </a:msub> <a:mo>/</a:mo> <a:msub> <a:mi>M</a:mi> <a:mo stretchy="false">⊙</a:mo> </a:msub> <a:mo>&gt;</a:mo> <a:mn>10</a:mn> </a:math> , and we explore measurements across a range of aperture sizes ( <d:math xmlns:d="http://www.w3.org/1998/Math/MathML" display="inline"> <d:msup> <d:mn>2.1</d:mn> <d:mo>′</d:mo> </d:msup> <d:mo>&lt;</d:mo> <d:msub> <d:mi>θ</d:mi> <d:mrow> <d:mi>ap</d:mi> </d:mrow> </d:msub> <d:mo>&lt;</d:mo> <d:msup> <d:mn>3.5</d:mn> <d:mo>′</d:mo> </d:msup> </d:math> ) and stellar mass selections. This statistic directly probes the velocity field of the large-scale structure, a unique observable of cosmic dynamics and modified gravity. In particular, at low redshifts, this quantity is especially interesting, as deviations from General Relativity are expected to be largest. Notably, our result represents the highest-significance low-redshift ( <f:math xmlns:f="http://www.w3.org/1998/Math/MathML" display="inline"> <f:mi>z</f:mi> <f:mo>∼</f:mo> <f:mn>0.3</f:mn> </f:math> ) detection of the kSZ pairwise effect yet. In our most optimal configuration ( <h:math xmlns:h="http://www.w3.org/1998/Math/MathML" display="inline"> <h:msub> <h:mi>θ</h:mi> <h:mrow> <h:mi>ap</h:mi> </h:mrow> </h:msub> <h:mo>=</h:mo> <h:msup> <h:mn>3.3</h:mn> <h:mo>′</h:mo> </h:msup> </h:math> , <j:math xmlns:j="http://www.w3.org/1998/Math/MathML" display="inline"> <j:mi>log</j:mi> <j:msub> <j:mi>M</j:mi> <j:mo>⋆</j:mo> </j:msub> <j:mo>&gt;</j:mo> <j:mn>11</j:mn> </j:math> ), we achieve a <l:math xmlns:l="http://www.w3.org/1998/Math/MathML" display="inline"> <l:mn>5</l:mn> <l:mi>σ</l:mi> </l:math> detection. Assuming that an estimate of the optical depth and galaxy bias of the sample exists via e.g., external observables, this measurement constrains the fundamental cosmological combination <n:math xmlns:n="http://www.w3.org/1998/Math/MathML" display="inline"> <n:msub> <n:mi>H</n:mi> <n:mn>0</n:mn> </n:msub> <n:mi>f</n:mi> <n:msubsup> <n:mi>σ</n:mi> <n:mn>8</n:mn> <n:mn>2</n:mn> </n:msubsup> </n:math> . A key challenge is the degeneracy with the galaxy optical depth. We address this by combining CMB lensing, which allows us to infer the halo mass and galaxy population properties, with hydrodynamical simulation estimates of the mean optical depth, <p:math xmlns:p="http://www.w3.org/1998/Math/MathML" display="inline"> <p:mover accent="true"> <p:mi>τ</p:mi> <p:mo stretchy="false">¯</p:mo> </p:mover> </p:math> . We stress that this is a proof-of-concept analysis; with BGS DR2 data we expect to improve the statistical precision by roughly a factor of two, paving the way toward robust tests of modified gravity with kSZ-informed velocity-field measurements at low redshift.