http://arxiv.org/abs/2203.12581
The field of millimetre-wave line-intensity mapping (LIM) is seeing increased experimental activity with pathfinder surveys already deployed or deploying in the next few years, making spectroscopic measurements of unresolved atomic and molecular line emission tracing the large-scale structure of the Universe. The next decade will also see the Rubin Observatory Legacy Survey of Space and Time (LSST) undertake a photometric galaxy survey programme of unprecedented scope, including measurements of cosmic shear exploiting weak gravitational lensing (WL) of background galaxies to map projected large-scale structure. We consider prospects for detecting angular cross power spectra between non-tomographic cosmic shear and mm-wave LIM surveys that measure emission from CO lines at $z=0.5$-$1$. We forecast that once the LSST Year 10 WL dataset is available, a future LIM experiment, conceivably deployed in the next 10-15 years, would enable such a cross-correlation detection with an overall signal-to-noise ratio of $50$, although the current pathfinder generation of CO/[C II] surveys are more likely to achieve a marginal $2\sigma$ detection against an earlier-stage LSST WL dataset. The signal has modest astrophysical constraining power yielding competitive constraints on cosmic molecular gas density at $z\lesssim1$, and degeneracies between astrophysical parameters and the intrinsic alignment amplitude mean that external information on either one could allow the cross-correlation analysis to significantly improve its constraints on the other.
D. Chung
Thu, 24 Mar 22
32/56
Comments: 12 pages + bibliography and appendix (15 pages total); 8 figures, 2 tables; submitted to MNRAS
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