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We present a power spectrum analysis of the ALMA Spectroscopic Survey LargeProgram (ASPECS LP) data from 84 to 115 GHz. These data predominantly probesmall-scale fluctuations ($k=10$-$100$ h Mpc$^{-1}$) in the aggregate COemission in galaxies at $1 \lesssim z \lesssim 4$. We place an integralconstraint on CO luminosity functions (LFs) in this redshift range via a directmeasurement of their second moments in the three-dimensional (3D) auto-powerspectrum, finding a total CO shot noise power$P_{\textrm{CO,CO}}(k_{\textrm{CO(2-1)}}) \leq 1.9\times10^2$ $\mu$K$^2$ (Mpch$^{-1}$)$^3$. This upper limit ($3\sigma$) is consistent with the observedASPECS CO LFs in Decarli et al. 2019, but rules out a large space in the rangeof $P_{\textrm{CO,CO}}(k_{\textrm{CO(2-1)}})$ inferred from these LFs, which weattribute primarily to large uncertainties in the normalization $\Phi_*$ andknee $L_*$ of the Schechter-form CO LFs at $z > 2$. Also, through powerspectrum analyses of ASPECS LP data with 415 positions from galaxies withavailable optical spectroscopic redshifts, we find that contributions to theobserved mean CO intensity and shot noise power of MUSE galaxies are largelyaccounted for by ASPECS blind detections, though there are $\sim20$%contributions to the CO(2-1) mean intensity due to sources previouslyundetected in the blind line search. Finally, we sum the fluxes from individualblind CO detections to yield a lower limit on the mean CO surface brightness at99 GHz of $\langle T_{\textrm{CO}} \rangle = 0.55\pm0.02$ $\mu$K, which weestimate represents $68$-$80$% of the total CO surface brightness at thisfrequency.

astrophysical journal/the astrophysical journal

The ALMA Spectroscopic Survey in the HUDF: Constraining cumulative CO  emission at $1 \lesssim z \lesssim 4$ with power spectrum analysis of ASPECS  LP data from 84 to 115 GHz