An Intensity Mapping Detection of Aggregate CO Line Emission at 3 mm

摘要: We present a detection of molecular gas emission at $z\sim1-5$ using the technique line intensity mapping. make use pair 3 mm interferometric data sets, first from ALMA Spectroscopic Survey in Hubble Ultra Deep Field (ASPECS), and second series Atacama Compact Array (ACA) observations conducted between 2016 2018, targeting COSMOS field. At 100 GHz, we measure non-zero power 97.8% 99.9% confidence ACA respectively. In joint result, reject zero-power hypothesis 99.99% confidence, finding $\tilde{I}^{2}_{s}(\nu)=770\pm210\ \mu\textrm{K}^2\ \textrm{Hz}\ \textrm{sr}$. After accounting for sample variance effects, estimated spectral shot is $\tilde{I}^{2}_{s}(\nu)=1010_{-390}^{+550}\ derive model various species our measurement expected to be sensitive to, estimate $120_{-40}^{+80}\ h^{-3}\,\textrm{Mpc}^{3}$, $200^{+120}_{-70}\ $90^{+70}_{-40}\ h^{-3}\,\textrm{Mpc}^{3}$ CO(2-1) $z=1.3$, CO(3-2) $z=2.5$, CO(4-3) $z=3.6$, Using ratios appropriate high-redshift galaxies, find these results good agreement with those CO Power Spectrum (COPSS). Adopting $\alpha_{\rm CO}=3.6\ M_{\odot}\ (\textrm{K}\ \textrm{km}\ \textrm{s}^{-1}\ \textrm{pc}^{2})^{-1}$, cosmic density $\rho_{\textrm{H}_2}(z)\sim 10^{8}\ \textrm{Mpc}^{-3}$ $z=1-3$.