COMAP Early Science: V. Constraints and Forecasts at \$z {\textbackslash}sim 3\$. Chung, D. T., Breysse, P. C., Cleary, K. A., Ihle, H. T., Padmanabhan, H., Silva, M. B., Bond, J. R., Borowska, J., Catha, M., Church, S. E., Dunne, D. A., Eriksen, H. K., Foss, M. K., Gaier, T., Gundersen, J. O., Harper, S. E., Harris, A. I., Hensley, B., Hobbs, R., Keating, L. C., Kim, J., Lamb, J. W., Lawrence, C. R., Lunde, J. G. S., Murray, N., Pearson, T. J., Philip, L., Rasmussen, M., Readhead, A. C. S., Rennie, T. J., Stutzer, N., Uzgil, B. D., Viero, M. P., Watts, D. J., Wechsler, R. H., Wehus, I. K., & Woody, D. P. arXiv:2111.05931 [astro-ph], November, 2021. arXiv: 2111.05931![COMAP Early Science: V. Constraints and Forecasts at \$z {\textbackslash}sim 3\$ [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex We present the current state of models for the \$z{\textbackslash}sim3\$ 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{\textbackslash},\$Mpc\${\textasciicircum}\{-1\}\$ represent the first direct 3D constraint on the clustering component of the CO(1-0) power spectrum. Our 95% upper limit on the redshift-space clustering amplitude \$A_\{{\textbackslash}rm clust\}{\textbackslash}lesssim70{\textbackslash},{\textbackslash}mu\$K\${\textasciicircum}2\$ greatly improves on the indirect upper limit of \$420{\textbackslash},{\textbackslash}mu\$K\${\textasciicircum}2\$ reported from the CO Power Spectrum Survey (COPSS) measurement at \$k{\textbackslash}sim1{\textbackslash},\$Mpc\${\textasciicircum}\{-1\}\$. The COMAP limit excludes a subset of models from previous literature, and constrains interpretation of the COPSS results, demonstrating the complementary nature of COMAP and interferometric CO surveys. Using line bias expectations from our priors, we also constrain the squared mean line intensity-bias product, \${\textbackslash}langle\{Tb\}{\textbackslash}rangle{\textasciicircum}2{\textbackslash}lesssim50{\textbackslash},{\textbackslash}mu\$K\${\textasciicircum}2\$, and the cosmic molecular gas density, \${\textbackslash}rho_{\textbackslash}text\{H2\}{\textless}2.5{\textbackslash}times10{\textasciicircum}8{\textbackslash},M_{\textbackslash}odot{\textbackslash},\$Mpc\${\textasciicircum}\{-3\}\$ (95% upper limits). Based on early instrument performance and our current CO signal estimates, we forecast that the five-year Pathfinder campaign will detect the CO power spectrum with overall signal-to-noise of 9-17. Between then and now, we also expect to detect the CO-galaxy cross-spectrum using overlapping galaxy survey data, enabling enhanced inferences of cosmic star-formation and galaxy-evolution history.
@article{chung_comap_2021,
title = {{COMAP} {Early} {Science}: {V}. {Constraints} and {Forecasts} at \$z {\textbackslash}sim 3\$},
shorttitle = {{COMAP} {Early} {Science}},
url = {http://arxiv.org/abs/2111.05931},
abstract = {We present the current state of models for the \$z{\textbackslash}sim3\$ 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{\textbackslash},\$Mpc\${\textasciicircum}\{-1\}\$ represent the first direct 3D constraint on the clustering component of the CO(1-0) power spectrum. Our 95\% upper limit on the redshift-space clustering amplitude \$A\_\{{\textbackslash}rm clust\}{\textbackslash}lesssim70{\textbackslash},{\textbackslash}mu\$K\${\textasciicircum}2\$ greatly improves on the indirect upper limit of \$420{\textbackslash},{\textbackslash}mu\$K\${\textasciicircum}2\$ reported from the CO Power Spectrum Survey (COPSS) measurement at \$k{\textbackslash}sim1{\textbackslash},\$Mpc\${\textasciicircum}\{-1\}\$. The COMAP limit excludes a subset of models from previous literature, and constrains interpretation of the COPSS results, demonstrating the complementary nature of COMAP and interferometric CO surveys. Using line bias expectations from our priors, we also constrain the squared mean line intensity-bias product, \${\textbackslash}langle\{Tb\}{\textbackslash}rangle{\textasciicircum}2{\textbackslash}lesssim50{\textbackslash},{\textbackslash}mu\$K\${\textasciicircum}2\$, and the cosmic molecular gas density, \${\textbackslash}rho\_{\textbackslash}text\{H2\}{\textless}2.5{\textbackslash}times10{\textasciicircum}8{\textbackslash},M\_{\textbackslash}odot{\textbackslash},\$Mpc\${\textasciicircum}\{-3\}\$ (95\% upper limits). Based on early instrument performance and our current CO signal estimates, we forecast that the five-year Pathfinder campaign will detect the CO power spectrum with overall signal-to-noise of 9-17. Between then and now, we also expect to detect the CO-galaxy cross-spectrum using overlapping galaxy survey data, enabling enhanced inferences of cosmic star-formation and galaxy-evolution history.},
urldate = {2021-12-07},
journal = {arXiv:2111.05931 [astro-ph]},
author = {Chung, Dongwoo T. and Breysse, Patrick C. and Cleary, Kieran A. and Ihle, Håvard T. and Padmanabhan, Hamsa and Silva, Marta B. and Bond, J. Richard and Borowska, Jowita and Catha, Morgan and Church, Sarah E. and Dunne, Delaney A. and Eriksen, Hans Kristian and Foss, Marie Kristine and Gaier, Todd and Gundersen, Joshua Ott and Harper, Stuart E. and Harris, Andrew I. and Hensley, Brandon and Hobbs, Richard and Keating, Laura C. and Kim, Junhan and Lamb, James W. and Lawrence, Charles R. and Lunde, Jonas Gahr Sturtzel and Murray, Norman and Pearson, Timothy J. and Philip, Liju and Rasmussen, Maren and Readhead, Anthony C. S. and Rennie, Thomas J. and Stutzer, Nils-Ole and Uzgil, Bade D. and Viero, Marco P. and Watts, Duncan J. and Wechsler, Risa H. and Wehus, Ingunn Kathrine and Woody, David P.},
month = nov,
year = {2021},
note = {arXiv: 2111.05931},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
}
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Constraints and Forecasts at \\$z {\\textbackslash}sim 3\\$","shorttitle":"COMAP Early Science","url":"http://arxiv.org/abs/2111.05931","abstract":"We present the current state of models for the \\$z{\\textbackslash}sim3\\$ 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{\\textbackslash},\\$Mpc\\${\\textasciicircum}\\{-1\\}\\$ represent the first direct 3D constraint on the clustering component of the CO(1-0) power spectrum. Our 95% upper limit on the redshift-space clustering amplitude \\$A_\\{{\\textbackslash}rm clust\\}{\\textbackslash}lesssim70{\\textbackslash},{\\textbackslash}mu\\$K\\${\\textasciicircum}2\\$ greatly improves on the indirect upper limit of \\$420{\\textbackslash},{\\textbackslash}mu\\$K\\${\\textasciicircum}2\\$ reported from the CO Power Spectrum Survey (COPSS) measurement at \\$k{\\textbackslash}sim1{\\textbackslash},\\$Mpc\\${\\textasciicircum}\\{-1\\}\\$. The COMAP limit excludes a subset of models from previous literature, and constrains interpretation of the COPSS results, demonstrating the complementary nature of COMAP and interferometric CO surveys. Using line bias expectations from our priors, we also constrain the squared mean line intensity-bias product, \\${\\textbackslash}langle\\{Tb\\}{\\textbackslash}rangle{\\textasciicircum}2{\\textbackslash}lesssim50{\\textbackslash},{\\textbackslash}mu\\$K\\${\\textasciicircum}2\\$, and the cosmic molecular gas density, \\${\\textbackslash}rho_{\\textbackslash}text\\{H2\\}{\\textless}2.5{\\textbackslash}times10{\\textasciicircum}8{\\textbackslash},M_{\\textbackslash}odot{\\textbackslash},\\$Mpc\\${\\textasciicircum}\\{-3\\}\\$ (95% upper limits). Based on early instrument performance and our current CO signal estimates, we forecast that the five-year Pathfinder campaign will detect the CO power spectrum with overall signal-to-noise of 9-17. Between then and now, we also expect to detect the CO-galaxy cross-spectrum using overlapping galaxy survey data, enabling enhanced inferences of cosmic star-formation and galaxy-evolution history.","urldate":"2021-12-07","journal":"arXiv:2111.05931 [astro-ph]","author":[{"propositions":[],"lastnames":["Chung"],"firstnames":["Dongwoo","T."],"suffixes":[]},{"propositions":[],"lastnames":["Breysse"],"firstnames":["Patrick","C."],"suffixes":[]},{"propositions":[],"lastnames":["Cleary"],"firstnames":["Kieran","A."],"suffixes":[]},{"propositions":[],"lastnames":["Ihle"],"firstnames":["Håvard","T."],"suffixes":[]},{"propositions":[],"lastnames":["Padmanabhan"],"firstnames":["Hamsa"],"suffixes":[]},{"propositions":[],"lastnames":["Silva"],"firstnames":["Marta","B."],"suffixes":[]},{"propositions":[],"lastnames":["Bond"],"firstnames":["J.","Richard"],"suffixes":[]},{"propositions":[],"lastnames":["Borowska"],"firstnames":["Jowita"],"suffixes":[]},{"propositions":[],"lastnames":["Catha"],"firstnames":["Morgan"],"suffixes":[]},{"propositions":[],"lastnames":["Church"],"firstnames":["Sarah","E."],"suffixes":[]},{"propositions":[],"lastnames":["Dunne"],"firstnames":["Delaney","A."],"suffixes":[]},{"propositions":[],"lastnames":["Eriksen"],"firstnames":["Hans","Kristian"],"suffixes":[]},{"propositions":[],"lastnames":["Foss"],"firstnames":["Marie","Kristine"],"suffixes":[]},{"propositions":[],"lastnames":["Gaier"],"firstnames":["Todd"],"suffixes":[]},{"propositions":[],"lastnames":["Gundersen"],"firstnames":["Joshua","Ott"],"suffixes":[]},{"propositions":[],"lastnames":["Harper"],"firstnames":["Stuart","E."],"suffixes":[]},{"propositions":[],"lastnames":["Harris"],"firstnames":["Andrew","I."],"suffixes":[]},{"propositions":[],"lastnames":["Hensley"],"firstnames":["Brandon"],"suffixes":[]},{"propositions":[],"lastnames":["Hobbs"],"firstnames":["Richard"],"suffixes":[]},{"propositions":[],"lastnames":["Keating"],"firstnames":["Laura","C."],"suffixes":[]},{"propositions":[],"lastnames":["Kim"],"firstnames":["Junhan"],"suffixes":[]},{"propositions":[],"lastnames":["Lamb"],"firstnames":["James","W."],"suffixes":[]},{"propositions":[],"lastnames":["Lawrence"],"firstnames":["Charles","R."],"suffixes":[]},{"propositions":[],"lastnames":["Lunde"],"firstnames":["Jonas","Gahr","Sturtzel"],"suffixes":[]},{"propositions":[],"lastnames":["Murray"],"firstnames":["Norman"],"suffixes":[]},{"propositions":[],"lastnames":["Pearson"],"firstnames":["Timothy","J."],"suffixes":[]},{"propositions":[],"lastnames":["Philip"],"firstnames":["Liju"],"suffixes":[]},{"propositions":[],"lastnames":["Rasmussen"],"firstnames":["Maren"],"suffixes":[]},{"propositions":[],"lastnames":["Readhead"],"firstnames":["Anthony","C.","S."],"suffixes":[]},{"propositions":[],"lastnames":["Rennie"],"firstnames":["Thomas","J."],"suffixes":[]},{"propositions":[],"lastnames":["Stutzer"],"firstnames":["Nils-Ole"],"suffixes":[]},{"propositions":[],"lastnames":["Uzgil"],"firstnames":["Bade","D."],"suffixes":[]},{"propositions":[],"lastnames":["Viero"],"firstnames":["Marco","P."],"suffixes":[]},{"propositions":[],"lastnames":["Watts"],"firstnames":["Duncan","J."],"suffixes":[]},{"propositions":[],"lastnames":["Wechsler"],"firstnames":["Risa","H."],"suffixes":[]},{"propositions":[],"lastnames":["Wehus"],"firstnames":["Ingunn","Kathrine"],"suffixes":[]},{"propositions":[],"lastnames":["Woody"],"firstnames":["David","P."],"suffixes":[]}],"month":"November","year":"2021","note":"arXiv: 2111.05931","keywords":"Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics","bibtex":"@article{chung_comap_2021,\n\ttitle = {{COMAP} {Early} {Science}: {V}. {Constraints} and {Forecasts} at \\$z {\\textbackslash}sim 3\\$},\n\tshorttitle = {{COMAP} {Early} {Science}},\n\turl = {http://arxiv.org/abs/2111.05931},\n\tabstract = {We present the current state of models for the \\$z{\\textbackslash}sim3\\$ 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{\\textbackslash},\\$Mpc\\${\\textasciicircum}\\{-1\\}\\$ represent the first direct 3D constraint on the clustering component of the CO(1-0) power spectrum. Our 95\\% upper limit on the redshift-space clustering amplitude \\$A\\_\\{{\\textbackslash}rm clust\\}{\\textbackslash}lesssim70{\\textbackslash},{\\textbackslash}mu\\$K\\${\\textasciicircum}2\\$ greatly improves on the indirect upper limit of \\$420{\\textbackslash},{\\textbackslash}mu\\$K\\${\\textasciicircum}2\\$ reported from the CO Power Spectrum Survey (COPSS) measurement at \\$k{\\textbackslash}sim1{\\textbackslash},\\$Mpc\\${\\textasciicircum}\\{-1\\}\\$. The COMAP limit excludes a subset of models from previous literature, and constrains interpretation of the COPSS results, demonstrating the complementary nature of COMAP and interferometric CO surveys. Using line bias expectations from our priors, we also constrain the squared mean line intensity-bias product, \\${\\textbackslash}langle\\{Tb\\}{\\textbackslash}rangle{\\textasciicircum}2{\\textbackslash}lesssim50{\\textbackslash},{\\textbackslash}mu\\$K\\${\\textasciicircum}2\\$, and the cosmic molecular gas density, \\${\\textbackslash}rho\\_{\\textbackslash}text\\{H2\\}{\\textless}2.5{\\textbackslash}times10{\\textasciicircum}8{\\textbackslash},M\\_{\\textbackslash}odot{\\textbackslash},\\$Mpc\\${\\textasciicircum}\\{-3\\}\\$ (95\\% upper limits). Based on early instrument performance and our current CO signal estimates, we forecast that the five-year Pathfinder campaign will detect the CO power spectrum with overall signal-to-noise of 9-17. Between then and now, we also expect to detect the CO-galaxy cross-spectrum using overlapping galaxy survey data, enabling enhanced inferences of cosmic star-formation and galaxy-evolution history.},\n\turldate = {2021-12-07},\n\tjournal = {arXiv:2111.05931 [astro-ph]},\n\tauthor = {Chung, Dongwoo T. and Breysse, Patrick C. and Cleary, Kieran A. and Ihle, Håvard T. and Padmanabhan, Hamsa and Silva, Marta B. and Bond, J. Richard and Borowska, Jowita and Catha, Morgan and Church, Sarah E. and Dunne, Delaney A. and Eriksen, Hans Kristian and Foss, Marie Kristine and Gaier, Todd and Gundersen, Joshua Ott and Harper, Stuart E. and Harris, Andrew I. and Hensley, Brandon and Hobbs, Richard and Keating, Laura C. and Kim, Junhan and Lamb, James W. and Lawrence, Charles R. and Lunde, Jonas Gahr Sturtzel and Murray, Norman and Pearson, Timothy J. and Philip, Liju and Rasmussen, Maren and Readhead, Anthony C. 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