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Joint Power Spectrum and Voxel Intensity Distribution Forecast on the CO Luminosity Function with COMAP

Ihle, H. T. and Chung, D. and Stein, G. and Alvarez, M. and Bond, J. R. and Breysse, P. C. and Cleary, K. A. and Eriksen, H. K. and Foss, M. K. and Gundersen, J. O. and Harper, S. and Murray, N. and Padmanabhan, H. and Viero, M. P. and Wehus, I. K. (2019) Joint Power Spectrum and Voxel Intensity Distribution Forecast on the CO Luminosity Function with COMAP. Astrophysical Journal, 871 (1). Art. No. 75. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20190123-100720504

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Abstract

We develop a framework for joint constraints on the CO luminosity function based on power spectra (PS) and voxel intensity distributions (VID) and apply this to simulations of CO Mapping Array Pathfinder (COMAP), a CO intensity mapping experiment. This Bayesian framework is based on a Markov chain Monte Carlo (MCMC) sampler coupled to a Gaussian likelihood with a joint PS + VID covariance matrix computed from a large number of fiducial simulations and re-calibrated with a small number of simulations per MCMC step. The simulations are based on dark matter halos from fast peak patch simulations combined with the L_(CO)(M_(halo)) model of Li et al. We find that the relative power to constrain the CO luminosity function depends on the luminosity range of interest. In particular, the VID is more sensitive at large luminosities, while the PS and the VID are both competitive at small and intermediate luminosities. The joint analysis is superior to using either observable separately. When averaging over CO luminosities ranging between L_(CO) = 10^4-10^7 L⊙, and over 10 cosmological realizations of COMAP Phase 2, the uncertainties (in dex) are larger by 58% and 30% for the PS and VID, respectively, when compared to the joint analysis (PS + VID). This method is generally applicable to any other random field, with a complicated likelihood, as long a fast simulation procedure is available.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aaf4bcDOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aaf4bcPublisherArticle
https://arxiv.org/abs/1808.07487arXivDiscussion Paper
ORCID:
AuthorORCID
Chung, D.0000-0003-2618-6504
Additional Information:© 2019 The American Astronomical Society. Received 2018 August 22; revised 2018 November 8; accepted 2018 November 27; published 2019 January 23. Support for the COMAP instrument and operation comes through the NSF cooperative agreement AST-1517598. Parts of this work were performed at the Jet Propulsion Laboratory (JPL) and California Institute of Technology, operating under a contract with the National Aeronautics and Space Administration. H.T.I., H.K.E., M.K.F., and I.K.W. acknowledge support from the Research Council of Norway through grant 251328. Research in Canada is supported by NSERC and CIFAR. These calculations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund—Research Excellence; and the University of Toronto. Work at Stanford University is supported by NSF AST-1517598 and by a seed grant from the Kavli Institute for Particle Astrophysics and Cosmology. J.O.G. acknowledges support from the Keck Institute for Space Studies, NSF AST-1517108, and the University of Miami. H.P.'s research is supported by the Tomalla Foundation. We thank Sarah E. Church, Tim Pearson, and other members of the COMAP collaboration for useful discussion and comments on a draft of this paper.
Group:Keck Institute for Space Studies
Funders:
Funding AgencyGrant Number
NSFAST-1517598
NASA/JPL/CaltechUNSPECIFIED
Research Council of Norway251328
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Canada Foundation for InnovationUNSPECIFIED
Compute CanadaUNSPECIFIED
Government of OntarioUNSPECIFIED
Ontario Research Fund-Research ExcellenceUNSPECIFIED
University of TorontoUNSPECIFIED
NSFAST-1517598
Kavli Institute for Particle Astrophysics and CosmologyUNSPECIFIED
Keck Institute for Space Studies (KISS)UNSPECIFIED
NSFAST-1517108
University of MiamiUNSPECIFIED
Tomalla FoundationUNSPECIFIED
Subject Keywords:diffuse radiation – galaxies: high-redshift – large-scale structure of universe
Record Number:CaltechAUTHORS:20190123-100720504
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20190123-100720504
Official Citation:H. T. Ihle et al 2019 ApJ 871 75
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:92422
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:23 Jan 2019 18:32
Last Modified:23 Jan 2019 18:32

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