COMAP Early Science. V. Constraints and Forecasts at z ∼ 3

@article{Chung2021COMAPES,
  title={COMAP Early Science. V. Constraints and Forecasts at z ∼ 3},
  author={Dongwoo T. Chung and Patrick C. Breysse and Kieran A. Cleary and H{\aa}vard T. Ihle and Hamsa Padmanabhan and Marta B. Silva and J. Richard Bond and Jowita Borowska and Morgan Catha and Sarah E. Church and Delaney A. Dunne and Hans Kristian Eriksen and Marie Kristine Foss and Todd Gaier and Joshua Ott Gundersen and Stuart E. Harper and Andrew I. Harris and Brandon S. Hensley and Richard Hobbs and Laura C. Keating and Junhan Kim and James W. Lamb and Charles R. Lawrence and Jonas Gahr Sturtzel Lunde and Norman W. Murray and Timothy J. Pearson and Liju Philip and Maren Rasmussen and Anthony C. S. Readhead and Thomas J. Rennie and Nils-Ole Stutzer and Bade D. Uzgil and Marco P. Viero and Duncan J. Watts and Risa H. Wechsler and Ingunn Kathrine Wehus and David P. Woody},
  journal={The Astrophysical Journal},
  year={2021},
  volume={933}
}
We present the current state of models for the z ∼ 3 carbon monoxide (CO) line intensity signal targeted by the CO Mapping Array Project (COMAP) Pathfinder in the context of its early science results. Our fiducial model, relating dark matter halo properties to CO luminosities, informs parameter priors with empirical models of the galaxy–halo connection and previous CO (1–0) observations. The Pathfinder early science data spanning wavenumbers k = 0.051–0.62 Mpc−1 represent the first direct 3D… 

COMAP Early Science. I. Overview

The CO Mapping Array Project (COMAP) aims to use line-intensity mapping of carbon monoxide (CO) to trace the distribution and global properties of galaxies over cosmic time, back to the Epoch of

COMAP Early Science. VII. Prospects for CO Intensity Mapping at Reionization

We introduce COMAP-EoR, the next generation of the Carbon Monoxide Mapping Array Project aimed at extending CO intensity mapping to the Epoch of Reionization. COMAP-EoR supplements the existing 30

COMAP Early Science. II. Pathfinder Instrument

Line intensity mapping (LIM) is a new technique for tracing the global properties of galaxies over cosmic time. Detection of the very faint signals from redshifted carbon monoxide (CO), a tracer of

COMAP Early Science. III. CO Data Processing

The first season COMAP analysis pipeline that converts raw detector readouts to calibrated sky maps is described, and one of the two scanning strategies is sensitive to residual instrumental systematics and is excluded from the Season 1 power spectrum estimates.

COMAP Early Science. IV. Power Spectrum Methodology and Results

We present the power spectrum methodology used for the first-season COMAP analysis, and assess the quality of the current data set. The main results are derived through the Feed–Feed

Analytical covariance between voxel intensity distributions and line-intensity mapping power spectra

The power spectrum and the voxel intensity distribution (VID) are two of the main proposed summary statistics to study line-intensity maps. We reformulate the derivation of the VID in terms of the

Unveiling cosmological information on small scales with line intensity mapping

One of the toughest challenges in modern cosmology is to probe the small scales k (cid:38)

References

SHOWING 1-10 OF 69 REFERENCES

COMAP Early Science. I. Overview

The CO Mapping Array Project (COMAP) aims to use line-intensity mapping of carbon monoxide (CO) to trace the distribution and global properties of galaxies over cosmic time, back to the Epoch of

COMAP Early Science. VII. Prospects for CO Intensity Mapping at Reionization

We introduce COMAP-EoR, the next generation of the Carbon Monoxide Mapping Array Project aimed at extending CO intensity mapping to the Epoch of Reionization. COMAP-EoR supplements the existing 30

COMAP Early Science. VI. A First Look at the COMAP Galactic Plane Survey

We present early results from the CO Mapping Array Project (COMAP) Galactic Plane Survey conducted between 2019 June and 2021 April, spanning 20° < ℓ < 40° in Galactic longitude and ∣b∣ < 1.°5 in

Constraining the CO intensity mapping power spectrum at intermediate redshifts

We compile available constraints on the carbon monoxide (CO) 1-0 luminosity functions and abundances at redshifts 0-3. This is used to develop a data driven halo model for the evolution of the CO

The ALMA Spectroscopic Survey in the HUDF: Constraining Cumulative CO Emission at 1 ≲ z ≲ 4 with Power Spectrum Analysis of ASPECS LP Data from 84 to 115 GHz

We present a power spectrum analysis of the ALMA Spectroscopic Survey Large Program (ASPECS LP) data from 84 to 115 GHz. These data predominantly probe small-scale fluctuations (k = 10–100 h Mpc−1)

COMAP Early Science. II. Pathfinder Instrument

Line intensity mapping (LIM) is a new technique for tracing the global properties of galaxies over cosmic time. Detection of the very faint signals from redshifted carbon monoxide (CO), a tracer of

On Estimating the Cosmic Molecular Gas Density from CO Line Intensity Mapping Observations

The Millimeter-wave Intensity Mapping Experiment (mmIME) recently reported a detection of excess spatial fluctuations at a wavelength of 3 mm, which can be attributed to unresolved emission of

An Intensity Mapping Constraint on the CO-galaxy Cross-power Spectrum at Redshift ∼3

The abundance of cold molecular gas plays a crucial role in models of galaxy evolution. While deep spectroscopic surveys of CO emission lines have been a primary tool for measuring this abundance,

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

We present a detection of molecular gas emission at z ∼ 1–5 using the technique of line intensity mapping. We make use of a pair of 3 mm interferometric data sets, the first from the Atacama Large

CO excitation of normal star forming galaxies out to $z=1.5$ as regulated by the properties of their interstellar medium

We investigate the CO excitation of normal star forming disk galaxies at z=1.5 using IRAM PdBI observations of the CO[2-1], CO[3-2] and CO[5-4] transitions for 4 galaxies, including VLA observations
...