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149 results on '"BOND, J. A."'

1. The Atacama Cosmology Telescope: Cosmology from Cross-correlations of unWISE Galaxies and ACT DR6 CMB Lensing.

Author

Farren, Gerrit S., Krolewski, Alex, MacCrann, Niall, Ferraro, Simone, Abril-Cabezas, Irene, An, Rui, Atkins, Zachary, Battaglia, Nicholas, Bond, J. Richard, Calabrese, Erminia, Choi, Steve K., Darwish, Omar, Devlin, Mark J., Duivenvoorden, Adriaan J., Dunkley, Jo, Hill, J. Colin, Hilton, Matt, Huffenberger, Kevin M., Kim, Joshua, and Louis, Thibaut

Subjects
PHYSICAL cosmology, LARGE scale structure (Astronomy), GALAXIES, TELESCOPES, COSMIC background radiation, UNITS of measurement, REDSHIFT
Abstract

We present tomographic measurements of structure growth using cross-correlations of Atacama Cosmology Telescope (ACT) DR6 and Planck cosmic microwave background (CMB) lensing maps with the unWISE Blue and Green galaxy samples, which span the redshift ranges 0.2 ≲ z ≲ 1.1 and 0.3 ≲ z ≲ 1.8, respectively. We improve on prior unWISE cross-correlations not just by making use of the new, high-precision ACT DR6 lensing maps, but also by including additional spectroscopic data for redshift calibration and by analyzing our measurements with a more flexible theoretical model. We determine the amplitude of matter fluctuations at low redshifts (z ≃ 0.2–1.6), finding S 8 ≡ σ 8 (Ω m / 0.3) 0.5 = 0.813 ± 0.021 using the ACT cross-correlation alone and S 8 = 0.810 ± 0.015 with a combination of Planck and ACT cross-correlations; these measurements are fully consistent with the predictions from primary CMB measurements assuming standard structure growth. The addition of baryon acoustic oscillation data breaks the degeneracy between σ 8 and Ω m , allowing us to measure σ 8 = 0.813 ± 0.020 from the cross-correlation of unWISE with ACT and σ 8 = 0.813 ± 0.015 from the combination of cross-correlations with ACT and Planck. These results also agree with the expectations from primary CMB extrapolations in ΛCDM cosmology; the consistency of σ 8 derived from our two redshift samples at z ∼ 0.6 and 1.1 provides a further check of our cosmological model. Our results suggest that structure formation on linear scales is well described by ΛCDM even down to low redshifts z ≲ 1. [ABSTRACT FROM AUTHOR]

Published
2024
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2. COMAP Early Science. VIII. A Joint Stacking Analysis with eBOSS Quasars.

Author

Dunne, Delaney A., Cleary, Kieran A., Breysse, Patrick C., Chung, Dongwoo T., Ihle, Håvard T., Bond, J. Richard, Eriksen, Hans Kristian, Gundersen, Joshua Ott, Keating, Laura C., Kim, Junhan, Lunde, Jonas Gahr Sturtzel, Murray, Norman, Padmanabhan, Hamsa, Philip, Liju, Stutzer, Nils-Ole, Tolgay, Doğa, Wehus, Ingunn Katherine, Church, Sarah E., Gaier, Todd, and Harris, Andrew I.

Subjects
QUASARS, GALACTIC redshift, REDSHIFT, RADIO astronomy
Abstract

We present a new upper limit on the cosmic molecular gas density at z = 2.4–3.4 obtained using the first year of observations from the CO Mapping Array Project (COMAP). COMAP data cubes are stacked on the 3D positions of 243 quasars selected from the Extended Baryon Oscillation Spectroscopic Survey (eBOSS) catalog, yielding a 95% upper limit for flux from CO(1–0) line emission of 0.129 Jy km s−1. Depending on the balance of the emission between the quasar host and its environment, this value can be interpreted as an average CO line luminosity L CO ′ of eBOSS quasars of ≤1.26 × 1011 K km pc2 s−1, or an average molecular gas density ρ H 2 in regions of the Universe containing a quasar of ≤1.52 × 108 M ⊙ cMpc−3. The L CO ′ upper limit falls among CO line luminosities obtained from individually targeted quasars in the COMAP redshift range, and the ρ H 2 value is comparable to upper limits obtained from other line intensity mapping (LIM) surveys and their joint analyses. Further, we forecast the values obtainable with the COMAP/eBOSS stack after the full 5 yr COMAP Pathfinder survey. We predict that a detection is probable with this method, depending on the CO properties of the quasar sample. Based on the achieved sensitivity, we believe that this technique of stacking LIM data on the positions of traditional galaxy or quasar catalogs is extremely promising, both as a technique for investigating large galaxy catalogs efficiently at high redshift and as a technique for bolstering the sensitivity of LIM experiments, even with a fraction of their total expected survey data. [ABSTRACT FROM AUTHOR]

Published
2024
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3. The Simons Observatory: a new open-source power spectrum pipeline applied to the Planck legacy data

Author

Li, Zack, primary, Louis, Thibaut, additional, Calabrese, Erminia, additional, Jense, Hidde, additional, Alonso, David, additional, Atkins, Zachary, additional, Bond, J. Richard, additional, Choi, Steve K., additional, Dunkley, Jo, additional, Fabbian, Giulio, additional, Garrido, Xavier, additional, H. Jaffe, Andrew, additional, Madhavacheril, Mathew S., additional, Meerburg, P. Daniel, additional, Natale, Umberto, additional, and Qu, Frank J., additional

Published
2023
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4. The Atacama Cosmology Telescope: limits on dark matter-baryon interactions from DR4 power spectra

Author

Li, Zack, primary, An, Rui, additional, Gluscevic, Vera, additional, Boddy, Kimberly K., additional, Bond, J. Richard, additional, Calabrese, Erminia, additional, Dunkley, Jo, additional, Gallardo, Patricio A., additional, Guan, Yilun, additional, Hincks, Adam, additional, Huffenberger, Kevin M., additional, Kosowsky, Arthur, additional, Louis, Thibaut, additional, Madhavacheril, Mathew S., additional, Moodley, Kavilan, additional, Page, Lyman A., additional, Partridge, Bruce, additional, Qu, Frank J., additional, Salatino, Maria, additional, Sherwin, Blake, additional, Sifón, Cristóbal, additional, Vargas, Cristian, additional, and Wollack, Edward J., additional

Published
2023
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5. Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

Author

Adhikari, Susmita, Shin, Tae-hyeon, Jain, Bhuvnesh, Hilton, Matt, Baxter, Eric, Chang, Chihway, Wechsler, Risa H., Battaglia, Nick, Bond, J. Richard, Bocquet, Sebastian, DeRose, Joseph, Choi, Steve K., Devlin, Mark, Dunkley, Jo, Evrard, August E., Ferraro, Simone, Hill, J. Colin, Hughes, John P., Gallardo, Patricio A., Lokken, Martine, MacInnis, Amanda, McMahon, Jeffrey, Madhavacheril, Mathew S., Nati, Frederico, Newburgh, Laura B., Niemack, Michael D., Page, Lyman A., Palmese, Antonella, Partridge, Bruce, Rozo, Eduardo, Rykoff, Eli, Salatino, Maria, Schillaci, Alessandro, Sehgal, Neelima, Sif��n, Crist��bal, To, Chun-Hao, Wollack, Ed, Wu, Hao-Yi, Xu, Zhilei, Aguena, Michel, Allam, Sahar, Amon, Alexandra, Annis, James, Avila, Santiago, Bacon, David, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Burke, David L., Rosell, Aurelio C., Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Choi, Ami, Costanzi, Matteo, da Costa, Luiz N., De Vicente, Juan, Desai, Shantanu, Diehl, Thomas H., Doel, Peter, Everett, Spencer, Ferrero, Ismael, Fert��, Agn��s, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Garc��a-Bellido, Juan, Gaztanaga, Enrique, Gruen, Daniel, Gruendl, Robert A., Gschwend, Julia, Gutierrez, Gaston, Hartley, Will G., Hinton, Samuel R., Hollowood, Devon L., Honscheid, Klaus, James, David J., Jeltema, Tesla, Kuehn, Kyler, Kuropatkin, Nikolay, Lahav, Ofer, Lima, Marcos, Maia, Marcio A. G., Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Ogando, Ricardo L. C., Paz-Chinch��n, Francisco, Malag��n, Andr��s Plazas, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Suchyta, Eric, Swanson, Molly E. C., Varga, Tamas N., Wilkinson, Reese D., Zhang, Yuanyuan, Austermann, Jason E., Beall, James A., Becker, Daniel T., Denison, Edward V., Duff, Shannon M., Hilton, Gene C., Hubmayr, Johannes, Ullom, Joel N., Van Lanen, Jeff, Vale, Leila R., Collaboration, DES, Collaboration, ACT, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), Adhikari, S, Shin, T, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, R, Battaglia, N, Bond, J, Bocquet, S, Choi, S, Derose, J, Devlin, M, Dunkley, J, Evrard, A, Ferraro, S, Hill, J, Hughes, J, Gallardo, P, Lokken, M, Macinnis, A, Madhavacheril, M, Mcmahon, J, Nati, F, Newburgh, L, Niemack, M, Page, L, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, To, C, Wollack, E, Wu, H, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, D, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, A, Costanzi, M, Da Costa, L, Vicente, J, Desai, S, Diehl, T, Doel, P, Everett, S, Ferrero, I, Ferte, A, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, R, Gschwend, J, Gutierrez, G, Hartley, W, Hinton, S, Hollowood, D, Honscheid, K, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M, Marshall, J, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchon, F, Malagon, A, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, E. C. Swanson, M, Varga, T, Wilkinson, R, Zhang, Y, Austermann, J, Beall, J, Becker, D, Denison, E, Duff, S, Hilton, G, Hubmayr, J, Ullom, J, Lanen, J, Vale, L, Adhikari, S., Shin, T. -H., Jain, B., Hilton, M., Baxter, E., Chang, C., Wechsler, R. H., Battaglia, N., Bond, J. R., Bocquet, S., Choi, S. K., Derose, J., Devlin, M., Dunkley, J., Evrard, A. E., Ferraro, S., Hill, J. C., Hughes, J. P., Gallardo, P. A., Lokken, M., Macinnis, A., Madhavacheril, M. S., Mcmahon, J., Nati, F., Newburgh, L. B., Niemack, M. D., Page, L. A., Palmese, A., Partridge, B., Rozo, E., Rykoff, E., Salatino, M., Schillaci, A., Sehgal, N., Sifon, C., C. -H., To, Wollack, E., H. -Y., Wu, Xu, Z., Aguena, M., Allam, S., Amon, A., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. C., Kind, M. C., Carretero, J., Castander, F. J., Choi, A., Costanzi, M., Da Costa, L. N., Vicente, J. D., Desai, S., Diehl, T. H., Doel, P., Everett, S., Ferrero, I., Ferte, A., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., L. C. Ogando R., Paz-Chinchon, F., Malagon, A. P., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., E. C. Swanson M., Varga, T. N., Wilkinson, R. D., Zhang, Y., Austermann, J. E., Beall, J. A., Becker, D. T., Denison, E. V., Duff, S. M., Hilton, G. C., Hubmayr, J., Ullom, J. N., Lanen, J. V., and Vale, L. R.

Subjects
Galaxy dark matter halos, 010308 nuclear & particles physics, FOS: Physical sciences, Cold dark matter, Astronomy and Astrophysics, Galaxy clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology, SZ effect, Galaxy cluster, Surveys, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxy evolution, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy kinematics
Abstract

Adhikari, S., et al. (DES and ACT Collaboration), We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev-Zel'dovich effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius is consistent with CDM-only simulations and is located at 2.4-0.4+0.3 Mpc h-1. We split the galaxies on color and find significant differences in their profile shapes. Red and green-valley galaxies show a splashback-like minimum in their slope profile consistent with theory, while the bluest galaxies show a weak feature at a smaller radius. We develop a mapping of galaxies to subhalos in simulations and assign colors based on infall time onto their hosts. We find that the shift in location of the steepest slope and different profile shapes can be mapped to the average time of infall of galaxies of different colors. The steepest slope traces a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in clusters over 3.2 Gyr, green galaxies about 2.2 Gyr, while blue galaxies have been accreted most recently and have not reached apocenter. Using the full radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching occurs after a delay of about a gigayear and that galaxies quench rapidly thereafter with an exponential timescale of 0.6 Gyr., The DES Data Management System is supported by the NSF under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Unionʼs Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2)

Published
2021

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

Author

Breysse, Patrick C., Chung, Dongwoo T., Cleary, Kieran A., Ihle, HĂĄvard T., Padmanabhan, Hamsa, Silva, Marta B., Bond, J. Richard, Borowska, Jowita, Catha, Morgan, Church, Sarah E., Dunne, Delaney A., Eriksen, Hans Kristian, Foss, Marie Kristine, Gaier, Todd, Gundersen, Joshua Ott, Harris, Andrew I., Hobbs, Richard, Keating, Laura, Lamb, James W., and Lawrence, Charles R.

Subjects
SIGNAL-to-noise ratio, CROSS correlation, CARBON monoxide, POWER spectra, COSMIC background radiation
Abstract

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 GHz COMAP Pathfinder with two additional 30 GHz instruments and a new 16 GHz receiver. This combination of frequencies will be able to simultaneously map CO(1â€"0) and CO(2â€"1) at reionization redshifts (z ∼ 5â€"8) in addition to providing a significant boost to the z ∼ 3 sensitivity of the Pathfinder. We examine a set of existing models of the EoR CO signal, and find power spectra spanning several orders of magnitude, highlighting our extreme ignorance about this period of cosmic history and the value of the COMAP- EoR measurement. We carry out the most detailed forecast to date of an intensity mapping cross correlation, and find that five out of the six models we consider yield signal to noise ratios (S/Ns) ≳ 20 for COMAP- EoR, with the brightest reaching a S/N above 400. We show that, for these models, COMAP- EoR can make a detailed measurement of the cosmic molecular gas history from z ∼ 2â€"8, as well as probe the population of faint, star-forming galaxies predicted by these models to be undetectable by traditional surveys. We show that, for the single model that does not predict numerous faint emitters, a COMAP- EoR -type measurement is required to rule out their existence. We briefly explore prospects for a third-generation Expanded Reionization Array (COMAP- ERA) capable of detecting the faintest models and characterizing the brightest signals in extreme detail. [ABSTRACT FROM AUTHOR]

Published
2022
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7. COMAP Early Science. V. Constraints and Forecasts at z ∼ 3.

Author

Chung, Dongwoo T., Breysse, Patrick C., Cleary, Kieran A., Ihle, HĂĄvard T., Padmanabhan, Hamsa, Silva, Marta B., Richard Bond, J., Borowska, Jowita, Catha, Morgan, Church, Sarah E., Dunne, Delaney A., Kristian Eriksen, Hans, Kristine Foss, Marie, Gaier, Todd, Ott Gundersen, Joshua, Harper, Stuart E., Harris, Andrew I., Hensley, Brandon, Hobbs, Richard, and Keating, Laura C.

Subjects
PROPERTIES of matter, GALACTIC evolution, POWER spectra, CARBON monoxide, GALAXY formation, REDSHIFT
Abstract

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 galaxyâ€"halo connection and previous CO (1â€"0) observations. The Pathfinder early science data spanning wavenumbers k = 0.051â€"0.62 Mpcâˆ'1 represent the first direct 3D constraint on the clustering component of the CO (1â€"0) power spectrum. Our 95% upper limit on the redshift-space clustering amplitude A clust ≲ 70 ÎĽ K2 greatly improves on the indirect upper limit of 420 ÎĽ K2 reported from the CO Power Spectrum Survey (COPSS) measurement at k ∼ 1 Mpcâˆ'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 intensityâ€"bias product, Tb 2 ≲ 50 ÎĽ K2, and the cosmic molecular gas density, ρ H2 < 2.5 Ă— 108 M ⊙ Mpcâˆ'3 (95% upper limits). Based on early instrument performance and our current CO signal estimates, we forecast that the 5 yr Pathfinder campaign will detect the CO power spectrum with overall signal-to-noise ratio of 9â€"17. Between then and now, we also expect to detect the COâ€"galaxy cross-spectrum using overlapping galaxy survey data, enabling enhanced inferences of cosmic star formation and galaxy evolution history. [ABSTRACT FROM AUTHOR]

Published
2022
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8. COMAP Early Science. II. Pathfinder Instrument.

Author

Lamb, James W., Cleary, Kieran A., Woody, David P., Catha, Morgan, Chung, Dongwoo T., Gundersen, Joshua Ott, Harper, Stuart E., Harris, Andrew I., Hobbs, Richard, Ihle, HĂĄvard T., Kocz, Jonathon, Pearson, Timothy J., Philip, Liju, Powell, Travis W., Basoalto, Lilian, Bond, J. Richard, Borowska, Jowita, Breysse, Patrick C., Church, Sarah E., and Dickinson, Clive

Subjects
FOCAL planes, CARBON monoxide, STAR formation, GALAXY clusters, RADIO telescopes
Abstract

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 star formation, pushes the limits of what is feasible with a total-power instrument. The CO Mapping Project Pathfinder is a first-generation instrument aiming to prove the concept and develop the technology for future experiments, as well as delivering early science products. With 19 receiver channels in a hexagonal focal plane arrangement on a 10.4 m antenna and an instantaneous 26â€"34 GHz frequency range with 2 MHz resolution, it is ideally suited to measuring CO (J = 1â€"0) from z ∼ 3. In this paper we discuss strategies for designing and building the Pathfinder and the challenges that were encountered. The design of the instrument prioritized LIM requirements over those of ancillary science. After a couple of years of operation, the instrument is well understood, and the first year of data is already yielding useful science results. Experience with this Pathfinder will guide the design of the next generations of experiments. [ABSTRACT FROM AUTHOR]

Published
2022
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9. COMAP Early Science. III. CO Data Processing.

Author

Foss, Marie K., Ihle, HĂĄvard T., Borowska, Jowita, Cleary, Kieran A., Eriksen, Hans Kristian, Harper, Stuart E., Kim, Junhan, Lamb, James W., Lunde, Jonas G. S., Philip, Liju, Rasmussen, Maren, Stutzer, Nils-Ole, Uzgil, Bade D., Watts, Duncan J., Wehus, Ingunn K., Woody, David P., Bond, J. Richard, Breysse, Patrick C., Catha, Morgan, and Church, Sarah E.

Subjects
ELECTRONIC data processing, STAR maps (Astronomy), WHITE noise, POWER spectra, DATA binning, CARTOGRAPHY
Abstract

We describe the first-season CO Mapping Array Project (COMAP) analysis pipeline that converts raw detector readouts to calibrated sky maps. This pipeline implements four main steps: gain calibration, filtering, data selection, and mapmaking. Absolute gain calibration relies on a combination of instrumental and astrophysical sources, while relative gain calibration exploits real-time total-power variations. High-efficiency filtering is achieved through spectroscopic common-mode rejection within and across receivers, resulting in nearly uncorrelated white noise within single-frequency channels. Consequently, near-optimal but biased maps are produced by binning the filtered time stream into pixelized maps; the corresponding signal bias transfer function is estimated through simulations. Data selection is performed automatically through a series of goodness-of-fit statistics, including χ 2 and multiscale correlation tests. Applying this pipeline to the first-season COMAP data, we produce a data set with very low levels of correlated noise. We find that one of our two scanning strategies (the Lissajous type) is sensitive to residual instrumental systematics. As a result, we no longer use this type of scan and exclude data taken this way from our Season 1 power spectrum estimates. We perform a careful analysis of our data processing and observing efficiencies and take account of planned improvements to estimate our future performance. Power spectrum results derived from the first-season COMAP maps are presented and discussed in companion papers. [ABSTRACT FROM AUTHOR]

Published
2022
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10. COMAP Early Science. IV. Power Spectrum Methodology and Results.

Author

Ihle, HĂĄvard T., Borowska, Jowita, Cleary, Kieran A., Eriksen, Hans Kristian, Foss, Marie K., Harper, Stuart E., Kim, Junhan, Lunde, Jonas G. S., Philip, Liju, Rasmussen, Maren, Stutzer, Nils-Ole, Uzgil, Bade D., Watts, Duncan J., Wehus, Ingunn Kathrine, Bond, J. Richard, Breysse, Patrick C., Catha, Morgan, Church, Sarah E., Chung, Dongwoo T., and Dickinson, Clive

Subjects
POWER spectra, TRANSFER functions, GALACTIC redshift, ELECTRONIC data processing, RADIO astronomy
Abstract

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 Feedâ€"Feed Pseudo-Cross-Spectrum (FPXS) method, which is a robust estimator with respect to both noise modeling errors and experimental systematics. We use effective transfer functions to take into account the effects of instrumental beam smoothing and various filter operations applied during the low-level data processing. The power spectra estimated in this way have allowed us to identify a systematic error associated with one of our two scanning strategies, believed to be due to residual ground or atmospheric contamination. We omit these data from our analysis and no longer use this scanning technique for observations. We present the power spectra from our first season of observing, and demonstrate that the uncertainties are integrating as expected for uncorrelated noise, with any residual systematics suppressed to a level below the noise. Using the FPXS method, and combining data on scales k = 0.051â€"0.62 Mpcâˆ'1, we estimate P CO(k) = âˆ'2. 7 ± 1.7 Ă— 104 ÎĽ K2 Mpc3, the first direct 3D constraint on the clustering component of the CO(1â€"0) power spectrum in the literature. [ABSTRACT FROM AUTHOR]

Published
2022
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11. Constraining ultralight axions with galaxy surveys

Author

Lagu��, Alex, Bond, J. Richard, Hlo��ek, Ren��e, Rogers, Keir K., Marsh, David J. E., and Grin, Daniel

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, High Energy Physics::Phenomenology, 0103 physical sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Ultralight axions and other bosons are dark matter candidates present in many high energy physics theories beyond the Standard Model. In particular, the string axiverse postulates the existence of up to $\mathcal{O}(100)$ light scalar bosons constituting the dark sector. Considering a mixture of axions and cold dark matter, we obtain upper bounds for the axion relic density $\Omega_a h^2 < 0.004$ for axions of mass $10^{-31}\;\mathrm{eV}\leq m_a \leq 10^{-26}\;\mathrm{eV}$ at 95% confidence. We also improve existing constraints by a factor of over 4.5 and 2.1 for axion masses of $10^{-25}$ eV and $10^{-32}$ eV, respectively. We use the Fourier-space galaxy clustering statistics from the Baryon Oscillation Spectroscopic Survey (BOSS) and demonstrate how galaxy surveys break important degeneracies in the axion parameter space compared to the cosmic microwave background (CMB). We test the validity of the effective field theory of large-scale structure approach to mixed ultralight axion dark matter by making our own mock galaxy catalogs and find an anisotropic ultralight axion signature in the galaxy quadrupole. We also observe an enhancement of the linear galaxy bias from 1.8 to 2.4 when allowing for 5% of the dark matter to be composed of a $10^{-28}$ eV axion in our simulations. Finally, we develop an augmented interpolation scheme allowing a fast computation of the axion contribution to the linear matter power spectrum leading to a 70% reduction of the computational cost for the full Monte Carlo Markov chains analysis., Comment: Updated references

Published
2022
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12. The Atacama Cosmology Telescope: DR4 maps and cosmological parameters

Author

Aiola, Simone, primary, Calabrese, Erminia, additional, Maurin, Loïc, additional, Naess, Sigurd, additional, Schmitt, Benjamin L., additional, Abitbol, Maximilian H., additional, Addison, Graeme E., additional, Ade, Peter A. R., additional, Alonso, David, additional, Amiri, Mandana, additional, Amodeo, Stefania, additional, Angile, Elio, additional, Austermann, Jason E., additional, Baildon, Taylor, additional, Battaglia, Nick, additional, Beall, James A., additional, Bean, Rachel, additional, Becker, Daniel T., additional, Bond, J Richard, additional, Bruno, Sarah Marie, additional, Calafut, Victoria, additional, Campusano, Luis E., additional, Carrero, Felipe, additional, Chesmore, Grace E., additional, Cho, Hsiao-mei, additional, Choi, Steve K., additional, Clark, Susan E., additional, Cothard, Nicholas F., additional, Crichton, Devin, additional, Crowley, Kevin T., additional, Darwish, Omar, additional, Datta, Rahul, additional, Denison, Edward V., additional, Devlin, Mark J., additional, Duell, Cody J., additional, Duff, Shannon M., additional, Duivenvoorden, Adriaan J., additional, Dunkley, Jo, additional, Dünner, Rolando, additional, Essinger-Hileman, Thomas, additional, Fankhanel, Max, additional, Ferraro, Simone, additional, Fox, Anna E., additional, Fuzia, Brittany, additional, Gallardo, Patricio A., additional, Gluscevic, Vera, additional, Golec, Joseph E., additional, Grace, Emily, additional, Gralla, Megan, additional, Guan, Yilun, additional, Hall, Kirsten, additional, Halpern, Mark, additional, Han, Dongwon, additional, Hargrave, Peter, additional, Hasselfield, Matthew, additional, Helton, Jakob M., additional, Henderson, Shawn, additional, Hensley, Brandon, additional, Hill, J. Colin, additional, Hilton, Gene C., additional, Hilton, Matt, additional, Hincks, Adam D., additional, Hložek, Renée, additional, Ho, Shuay-Pwu Patty, additional, Hubmayr, Johannes, additional, Huffenberger, Kevin M., additional, Hughes, John P., additional, Infante, Leopoldo, additional, Irwin, Kent, additional, Jackson, Rebecca, additional, Klein, Jeff, additional, Knowles, Kenda, additional, Koopman, Brian, additional, Kosowsky, Arthur, additional, Lakey, Vincent, additional, Li, Dale, additional, Li, Yaqiong, additional, Li, Zack, additional, Lokken, Martine, additional, Louis, Thibaut, additional, Lungu, Marius, additional, MacInnis, Amanda, additional, Madhavacheril, Mathew, additional, Maldonado, Felipe, additional, Mallaby-Kay, Maya, additional, Marsden, Danica, additional, McMahon, Jeff, additional, Menanteau, Felipe, additional, Moodley, Kavilan, additional, Morton, Tim, additional, Namikawa, Toshiya, additional, Nati, Federico, additional, Newburgh, Laura, additional, Nibarger, John P., additional, Nicola, Andrina, additional, Niemack, Michael D., additional, Nolta, Michael R., additional, Orlowski-Sherer, John, additional, Page, Lyman A., additional, Pappas, Christine G., additional, Partridge, Bruce, additional, Phakathi, Phumlani, additional, Pisano, Giampaolo, additional, Prince, Heather, additional, Puddu, Roberto, additional, Qu, Frank J., additional, Rivera, Jesus, additional, Robertson, Naomi, additional, Rojas, Felipe, additional, Salatino, Maria, additional, Schaan, Emmanuel, additional, Schillaci, Alessandro, additional, Sehgal, Neelima, additional, Sherwin, Blake D., additional, Sierra, Carlos, additional, Sievers, Jon, additional, Sifon, Cristobal, additional, Sikhosana, Precious, additional, Simon, Sara, additional, Spergel, David N., additional, Staggs, Suzanne T., additional, Stevens, Jason, additional, Storer, Emilie, additional, Sunder, Dhaneshwar D., additional, Switzer, Eric R., additional, Thorne, Ben, additional, Thornton, Robert, additional, Trac, Hy, additional, Treu, Jesse, additional, Tucker, Carole, additional, Vale, Leila R., additional, Engelen, Alexander Van, additional, Lanen, Jeff Van, additional, Vavagiakis, Eve M., additional, Wagoner, Kasey, additional, Wang, Yuhan, additional, Ward, Jonathan T., additional, Wollack, Edward J., additional, Xu, Zhilei, additional, Zago, Fernando, additional, and Zhu, Ningfeng, additional

Published
2020
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13. The Atacama Cosmology Telescope: a measurement of the Cosmic Microwave Background power spectra at 98 and 150 GHz

Author

Choi, Steve K., primary, Hasselfield, Matthew, additional, Ho, Shuay-Pwu Patty, additional, Koopman, Brian, additional, Lungu, Marius, additional, Abitbol, Maximilian H., additional, Addison, Graeme E., additional, Ade, Peter A. R., additional, Aiola, Simone, additional, Alonso, David, additional, Amiri, Mandana, additional, Amodeo, Stefania, additional, Angile, Elio, additional, Austermann, Jason E., additional, Baildon, Taylor, additional, Battaglia, Nick, additional, Beall, James A., additional, Bean, Rachel, additional, Becker, Daniel T., additional, Bond, J Richard, additional, Bruno, Sarah Marie, additional, Calabrese, Erminia, additional, Calafut, Victoria, additional, Campusano, Luis E., additional, Carrero, Felipe, additional, Chesmore, Grace E., additional, Cho, Hsiao-mei, additional, Clark, Susan E., additional, Cothard, Nicholas F., additional, Crichton, Devin, additional, Crowley, Kevin T., additional, Darwish, Omar, additional, Datta, Rahul, additional, Denison, Edward V., additional, Devlin, Mark J., additional, Duell, Cody J., additional, Duff, Shannon M., additional, Duivenvoorden, Adriaan J., additional, Dunkley, Jo, additional, Dünner, Rolando, additional, Essinger-Hileman, Thomas, additional, Fankhanel, Max, additional, Ferraro, Simone, additional, Fox, Anna E., additional, Fuzia, Brittany, additional, Gallardo, Patricio A., additional, Gluscevic, Vera, additional, Golec, Joseph E., additional, Grace, Emily, additional, Gralla, Megan, additional, Guan, Yilun, additional, Hall, Kirsten, additional, Halpern, Mark, additional, Han, Dongwon, additional, Hargrave, Peter, additional, Henderson, Shawn, additional, Hensley, Brandon, additional, Hill, J. Colin, additional, Hilton, Gene C., additional, Hilton, Matt, additional, Hincks, Adam D., additional, Hložek, Renée, additional, Hubmayr, Johannes, additional, Huffenberger, Kevin M., additional, Hughes, John P., additional, Infante, Leopoldo, additional, Irwin, Kent, additional, Jackson, Rebecca, additional, Klein, Jeff, additional, Knowles, Kenda, additional, Kosowsky, Arthur, additional, Lakey, Vincent, additional, Li, Dale, additional, Li, Yaqiong, additional, Li, Zack, additional, Lokken, Martine, additional, Louis, Thibaut, additional, MacInnis, Amanda, additional, Madhavacheril, Mathew, additional, Maldonado, Felipe, additional, Mallaby-Kay, Maya, additional, Marsden, Danica, additional, Maurin, Loïc, additional, McMahon, Jeff, additional, Menanteau, Felipe, additional, Moodley, Kavilan, additional, Morton, Tim, additional, Naess, Sigurd, additional, Namikawa, Toshiya, additional, Nati, Federico, additional, Newburgh, Laura, additional, Nibarger, John P., additional, Nicola, Andrina, additional, Niemack, Michael D., additional, Nolta, Michael R., additional, Orlowski-Sherer, John, additional, Page, Lyman A., additional, Pappas, Christine G., additional, Partridge, Bruce, additional, Phakathi, Phumlani, additional, Prince, Heather, additional, Puddu, Roberto, additional, Qu, Frank J., additional, Rivera, Jesus, additional, Robertson, Naomi, additional, Rojas, Felipe, additional, Salatino, Maria, additional, Schaan, Emmanuel, additional, Schillaci, Alessandro, additional, Schmitt, Benjamin L., additional, Sehgal, Neelima, additional, Sherwin, Blake D., additional, Sierra, Carlos, additional, Sievers, Jon, additional, Sifon, Cristobal, additional, Sikhosana, Precious, additional, Simon, Sara, additional, Spergel, David N., additional, Staggs, Suzanne T., additional, Stevens, Jason, additional, Storer, Emilie, additional, Sunder, Dhaneshwar D., additional, Switzer, Eric R., additional, Thorne, Ben, additional, Thornton, Robert, additional, Trac, Hy, additional, Treu, Jesse, additional, Tucker, Carole, additional, Vale, Leila R., additional, Engelen, Alexander Van, additional, Lanen, Jeff Van, additional, Vavagiakis, Eve M., additional, Wagoner, Kasey, additional, Wang, Yuhan, additional, Ward, Jonathan T., additional, Wollack, Edward J., additional, Xu, Zhilei, additional, Zago, Fernando, additional, and Zhu, Ningfeng, additional

Published
2020
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15. The cross correlation of the ABS and ACT maps

Author

Li, Zack, primary, Naess, Sigurd, additional, Aiola, Simone, additional, Alonso, David, additional, Appel, John W., additional, Bond, J. Richard, additional, Calabrese, Erminia, additional, Choi, Steve K., additional, Crowley, Kevin T., additional, Essinger-Hileman, Thomas, additional, Duff, Shannon M., additional, Dunkley, Joanna, additional, Fowler, J.W., additional, Gallardo, Patricio, additional, Ho, Shuay-Pwu Patty, additional, Hubmayr, Johannes, additional, Kusaka, Akito, additional, Louis, Thibaut, additional, Madhavacheril, Mathew S., additional, McMahon, Jeffrey, additional, Nati, Federico, additional, Niemack, Michael D., additional, Page, Lyman, additional, Parker, Lucas, additional, Partridge, Bruce, additional, Salatino, Maria, additional, Sievers, Jonathan L., additional, Sifón, Cristóbal, additional, Simon, Sara M., additional, Staggs, Suzanne T., additional, Storer, Emilie, additional, and Wollack, Edward J., additional

Published
2020
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16. A Simulation-based Method for Correcting Mode Coupling in CMB Angular Power Spectra.

Author

Leung, J. S.-Y., Hartley, J., Nagy, J. M., Netterfield, C. B., Shariff, J. A., Ade, P. A. R., Amiri, M., Benton, S. J., Bergman, A. S., Bihary, R., Bock, J. J., Bond, J. R., Bonetti, J. A., Bryan, S. A., Chiang, H. C., Contaldi, C. R., Doré, O., Duivenvoorden, A. J., Eriksen, H. K., and Farhang, M.

Subjects
POWER spectra, COSMIC background radiation, TRANSFER matrix, STAR maps (Astronomy), TRANSFER functions, WATER pipelines
Abstract

Modern cosmic microwave background (CMB) analysis pipelines regularly employ complex time-domain filters, beam models, masking, and other techniques during the production of sky maps and their corresponding angular power spectra. However, these processes can generate couplings between multipoles from the same spectrum and from different spectra, in addition to the typical power attenuation. Within the context of pseudo- C â„" based, MASTER-style analyses, the net effect of the time-domain filtering is commonly approximated by a multiplicative transfer function, F â„" , that can fail to capture mode mixing and is dependent on the spectrum of the signal. To address these shortcomings, we have developed a simulation-based spectral correction approach that constructs a two-dimensional transfer matrix, J â„" â„" ′ , which contains information about mode mixing in addition to mode attenuation. We demonstrate the application of this approach on data from the first flight of the Spider balloon-borne CMB experiment. [ABSTRACT FROM AUTHOR]

Published
2022
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17. A Constraint on Primordial B -modes from the First Flight of the Spider Balloon-borne Telescope.

Author

Ade, P. A. R., Amiri, M., Benton, S. J., Bergman, A. S., Bihary, R., Bock, J. J., Bond, J. R., Bonetti, J. A., Bryan, S. A., Chiang, H. C., Contaldi, C. R., Doré, O., Duivenvoorden, A. J., Eriksen, H. K., Farhang, M., Filippini, J. P., Fraisse, A. A., Freese, K., Galloway, M., and Gambrel, A. E.

Subjects
SPECTRAL energy distribution, COSMIC background radiation, SYNCHROTRON radiation, TEST reliability
Abstract

We present the first linear polarization measurements from the 2015 long-duration balloon flight of Spider, which is an experiment that is designed to map the polarization of the cosmic microwave background (CMB) on degree angular scales. The results from these measurements include maps and angular power spectra from observations of 4.8% of the sky at 95 and 150 GHz, along with the results of internal consistency tests on these data. While the polarized CMB anisotropy from primordial density perturbations is the dominant signal in this region of sky, Galactic dust emission is also detected with high significance. Galactic synchrotron emission is found to be negligible in the Spider bands. We employ two independent foreground-removal techniques to explore the sensitivity of the cosmological result to the assumptions made by each. The primary method uses a dust template derived from Planck data to subtract the Galactic dust signal. A second approach, which constitutes a joint analysis of Spider and Planck data in the harmonic domain, assumes a modified-blackbody model for the spectral energy distribution of the dust with no constraint on its spatial morphology. Using a likelihood that jointly samples the template amplitude and r parameter space, we derive 95% upper limits on the primordial tensor-to-scalar ratio from Feldmanâ€"Cousins and Bayesian constructions, finding r < 0.11 and r < 0.19, respectively. Roughly half the uncertainty in r derives from noise associated with the template subtraction. New data at 280 GHz from Spider ’s second flight will complement the Planck polarization maps, providing powerful measurements of the polarized Galactic dust emission. [ABSTRACT FROM AUTHOR]

Published
2022
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18. The Simons Observatory Large Aperture Telescope Receiver.

Author

Zhu, Ningfeng, Bhandarkar, Tanay, Coppi, Gabriele, Kofman, Anna M., Orlowski-Scherer, John L., Xu, Zhilei, Adachi, Shunsuke, Ade, Peter, Aiola, Simone, Austermann, Jason, Bazarko, Andrew O., Beall, James A., Bhimani, Sanah, Bond, J. Richard, Chesmore, Grace E., Choi, Steve K., Connors, Jake, Cothard, Nicholas F., Devlin, Mark, and Dicker, Simon

Published
2021
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19. The Atacama Cosmology Telescope: Detection of Millimeter-wave Transient Sources.

Author

Naess, Sigurd, Battaglia, Nick, Bond, J. Richard, Calabrese, Erminia, Choi, Steve K., Cothard, Nicholas F., Devlin, Mark, Duell, Cody J., Duivenvoorden, Adriaan J., Dunkley, Jo, Dünner, Rolando, Gallardo, Patricio A., Gralla, Megan, Guan, Yilun, Halpern, Mark, Hill, J. Colin, Hilton, Matt, Huffenberger, Kevin M., Koopman, Brian J., and Kosowsky, Arthur B.

Subjects
PHYSICAL cosmology, TELESCOPES, FLUX (Energy)
Abstract

We report on the serendipitous discovery of three transient millimeter-wave sources using data from the Atacama Cosmology Telescope. The first, detected at R.A. = 273.8138, decl. = −49.4628 at ∼50σ total, brightened from less than 5 mJy to at least 1100 mJy at 150 GHz with an unknown rise time shorter than 13 days, during which the increase from 250 mJy to 1100 mJy took only 8 minutes. Maximum flux was observed on 2019 November 8. The source's spectral index in flux between 90–150 GHz was positive, α = 1.5 ± 0.2. The second, detected at R.A. = 105.1584, decl. = −11.2434 at ∼20σ total, brightened from less than 20 mJy to at least 300 mJy at 150 GHz with an unknown rise time shorter than 8 days. Maximum flux was observed on 2019 December 15. Its spectral index was also positive, α = 1.8 ± 0.2. The third, detected at R.A. = 301.9952, decl. = 16.1652 at ∼40σ total, brightened from less than 8 mJy to at least 300 mJy at 150 GHz over a day or less but decayed over a few days. Maximum flux was observed on 2018 September 11. Its spectrum was approximately flat, with a spectral index of α = −0.2 ± 0.1. None of the sources were polarized to the limits of these measurements. The two rising-spectrum sources are coincident in position with M and K stars, while the third is coincident with a G star. [ABSTRACT FROM AUTHOR]

Published
2021
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20. The Atacama Cosmology Telescope: Summary of DR4 and DR5 Data Products and Data Access.

Author

Mallaby-Kay, Maya, Atkins, Zachary, Aiola, Simone, Amodeo, Stefania, Austermann, Jason E., Beall, James A., Becker, Daniel T., Bond, J. Richard, Calabrese, Erminia, Chesmore, Grace E., Choi, Steve K., Crowley, Kevin T., Darwish, Omar, Denison, Edward V., Devlin, Mark J., Duff, Shannon M., Duivenvoorden, Adriaan J., Dunkley, Jo, Ferraro, Simone, and Fichman, Kyra

Published
2021
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21. The Simons Observatory: science goals and forecasts

Author

Ade, Peter, primary, Aguirre, James, additional, Ahmed, Zeeshan, additional, Aiola, Simone, additional, Ali, Aamir, additional, Alonso, David, additional, Alvarez, Marcelo A., additional, Arnold, Kam, additional, Ashton, Peter, additional, Austermann, Jason, additional, Awan, Humna, additional, Baccigalupi, Carlo, additional, Baildon, Taylor, additional, Barron, Darcy, additional, Battaglia, Nick, additional, Battye, Richard, additional, Baxter, Eric, additional, Bazarko, Andrew, additional, Beall, James A., additional, Bean, Rachel, additional, Beck, Dominic, additional, Beckman, Shawn, additional, Beringue, Benjamin, additional, Bianchini, Federico, additional, Boada, Steven, additional, Boettger, David, additional, Bond, J. Richard, additional, Borrill, Julian, additional, Brown, Michael L., additional, Bruno, Sarah Marie, additional, Bryan, Sean, additional, Calabrese, Erminia, additional, Calafut, Victoria, additional, Calisse, Paolo, additional, Carron, Julien, additional, Challinor, Anthony, additional, Chesmore, Grace, additional, Chinone, Yuji, additional, Chluba, Jens, additional, Cho, Hsiao-Mei Sherry, additional, Choi, Steve, additional, Coppi, Gabriele, additional, Cothard, Nicholas F., additional, Coughlin, Kevin, additional, Crichton, Devin, additional, Crowley, Kevin D., additional, Crowley, Kevin T., additional, Cukierman, Ari, additional, D'Ewart, John M., additional, Dünner, Rolando, additional, de Haan, Tijmen, additional, Devlin, Mark, additional, Dicker, Simon, additional, Didier, Joy, additional, Dobbs, Matt, additional, Dober, Bradley, additional, Duell, Cody J., additional, Duff, Shannon, additional, Duivenvoorden, Adri, additional, Dunkley, Jo, additional, Dusatko, John, additional, Errard, Josquin, additional, Fabbian, Giulio, additional, Feeney, Stephen, additional, Ferraro, Simone, additional, Fluxà, Pedro, additional, Freese, Katherine, additional, Frisch, Josef C., additional, Frolov, Andrei, additional, Fuller, George, additional, Fuzia, Brittany, additional, Galitzki, Nicholas, additional, Gallardo, Patricio A., additional, Ghersi, Jose Tomas Galvez, additional, Gao, Jiansong, additional, Gawiser, Eric, additional, Gerbino, Martina, additional, Gluscevic, Vera, additional, Goeckner-Wald, Neil, additional, Golec, Joseph, additional, Gordon, Sam, additional, Gralla, Megan, additional, Green, Daniel, additional, Grigorian, Arpi, additional, Groh, John, additional, Groppi, Chris, additional, Guan, Yilun, additional, Gudmundsson, Jon E., additional, Han, Dongwon, additional, Hargrave, Peter, additional, Hasegawa, Masaya, additional, Hasselfield, Matthew, additional, Hattori, Makoto, additional, Haynes, Victor, additional, Hazumi, Masashi, additional, He, Yizhou, additional, Healy, Erin, additional, Henderson, Shawn W., additional, Hervias-Caimapo, Carlos, additional, Hill, Charles A., additional, Hill, J. Colin, additional, Hilton, Gene, additional, Hilton, Matt, additional, Hincks, Adam D., additional, Hinshaw, Gary, additional, Hložek, Renée, additional, Ho, Shirley, additional, Ho, Shuay-Pwu Patty, additional, Howe, Logan, additional, Huang, Zhiqi, additional, Hubmayr, Johannes, additional, Huffenberger, Kevin, additional, Hughes, John P., additional, Ijjas, Anna, additional, Ikape, Margaret, additional, Irwin, Kent, additional, Jaffe, Andrew H., additional, Jain, Bhuvnesh, additional, Jeong, Oliver, additional, Kaneko, Daisuke, additional, Karpel, Ethan D., additional, Katayama, Nobuhiko, additional, Keating, Brian, additional, Kernasovskiy, Sarah S., additional, Keskitalo, Reijo, additional, Kisner, Theodore, additional, Kiuchi, Kenji, additional, Klein, Jeff, additional, Knowles, Kenda, additional, Koopman, Brian, additional, Kosowsky, Arthur, additional, Krachmalnicoff, Nicoletta, additional, Kuenstner, Stephen E., additional, Kuo, Chao-Lin, additional, Kusaka, Akito, additional, Lashner, Jacob, additional, Lee, Adrian, additional, Lee, Eunseong, additional, Leon, David, additional, Leung, Jason S.-Y., additional, Lewis, Antony, additional, Li, Yaqiong, additional, Li, Zack, additional, Limon, Michele, additional, Linder, Eric, additional, Lopez-Caraballo, Carlos, additional, Louis, Thibaut, additional, Lowry, Lindsay, additional, Lungu, Marius, additional, Madhavacheril, Mathew, additional, Mak, Daisy, additional, Maldonado, Felipe, additional, Mani, Hamdi, additional, Mates, Ben, additional, Matsuda, Frederick, additional, Maurin, Loïc, additional, Mauskopf, Phil, additional, May, Andrew, additional, McCallum, Nialh, additional, McKenney, Chris, additional, McMahon, Jeff, additional, Meerburg, P. Daniel, additional, Meyers, Joel, additional, Miller, Amber, additional, Mirmelstein, Mark, additional, Moodley, Kavilan, additional, Munchmeyer, Moritz, additional, Munson, Charles, additional, Naess, Sigurd, additional, Nati, Federico, additional, Navaroli, Martin, additional, Newburgh, Laura, additional, Nguyen, Ho Nam, additional, Niemack, Michael, additional, Nishino, Haruki, additional, Orlowski-Scherer, John, additional, Page, Lyman, additional, Partridge, Bruce, additional, Peloton, Julien, additional, Perrotta, Francesca, additional, Piccirillo, Lucio, additional, Pisano, Giampaolo, additional, Poletti, Davide, additional, Puddu, Roberto, additional, Puglisi, Giuseppe, additional, Raum, Chris, additional, Reichardt, Christian L., additional, Remazeilles, Mathieu, additional, Rephaeli, Yoel, additional, Riechers, Dominik, additional, Rojas, Felipe, additional, Roy, Anirban, additional, Sadeh, Sharon, additional, Sakurai, Yuki, additional, Salatino, Maria, additional, Rao, Mayuri Sathyanarayana, additional, Schaan, Emmanuel, additional, Schmittfull, Marcel, additional, Sehgal, Neelima, additional, Seibert, Joseph, additional, Seljak, Uros, additional, Sherwin, Blake, additional, Shimon, Meir, additional, Sierra, Carlos, additional, Sievers, Jonathan, additional, Sikhosana, Precious, additional, Silva-Feaver, Maximiliano, additional, Simon, Sara M., additional, Sinclair, Adrian, additional, Siritanasak, Praween, additional, Smith, Kendrick, additional, Smith, Stephen R., additional, Spergel, David, additional, Staggs, Suzanne T., additional, Stein, George, additional, Stevens, Jason R., additional, Stompor, Radek, additional, Suzuki, Aritoki, additional, Tajima, Osamu, additional, Takakura, Satoru, additional, Teply, Grant, additional, Thomas, Daniel B., additional, Thorne, Ben, additional, Thornton, Robert, additional, Trac, Hy, additional, Tsai, Calvin, additional, Tucker, Carole, additional, Ullom, Joel, additional, Vagnozzi, Sunny, additional, Engelen, Alexander van, additional, Lanen, Jeff Van, additional, Winkle, Daniel D. Van, additional, Vavagiakis, Eve M., additional, Vergès, Clara, additional, Vissers, Michael, additional, Wagoner, Kasey, additional, Walker, Samantha, additional, Ward, Jon, additional, Westbrook, Ben, additional, Whitehorn, Nathan, additional, Williams, Jason, additional, Williams, Joel, additional, Wollack, Edward J., additional, Xu, Zhilei, additional, Yu, Byeonghee, additional, Yu, Cyndia, additional, Zago, Fernando, additional, Zhang, Hezi, additional, and Zhu, Ningfeng, additional

Published
2019
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22. The Atacama Cosmology Telescope: Weighing Distant Clusters with the Most Ancient Light.

Author

Madhavacheril, Mathew S., Sifón, Cristóbal, Battaglia, Nicholas, Aiola, Simone, Amodeo, Stefania, Austermann, Jason E., Beall, James A., Becker, Daniel T., Bond, J. Richard, Calabrese, Erminia, Choi, Steve K., Denison, Edward V., Devlin, Mark J., Dicker, Simon R., Duff, Shannon M., Duivenvoorden, Adriaan J., Dunkley, Jo, Dünner, Rolando, Ferraro, Simone, and Gallardo, Patricio A.

Published
2020
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23. Atacama Cosmology Telescope: Dusty Star-forming Galaxies and Active Galactic Nuclei in the Equatorial Survey.

Author

Gralla, Megan B., Marriage, Tobias A., Addison, Graeme, Baker, Andrew J., Bond, J. Richard, Crichton, Devin, Datta, Rahul, Devlin, Mark J., Dunkley, Joanna, Dünner, Rolando, Fowler, Joseph, Gallardo, Patricio A., Hall, Kirsten, Halpern, Mark, Hasselfield, Matthew, Hilton, Matt, Hincks, Adam D., Huffenberger, Kevin M., Hughes, John P., and Kosowsky, Arthur

Subjects
ACTIVE galaxies, PHYSICAL cosmology, ACTINIC flux, TELESCOPES, ACTIVE galactic nuclei
Abstract

We present a catalog of 510 radio-loud active galactic nuclei (AGNs, primarily blazars) and 287 dusty star-forming galaxies (DSFGs) detected by the Atacama Cosmology Telescope at significance in frequency bands centered on 148 GHz (2 mm), 218 GHz (1.4 mm), and 277 GHz (1.1 mm), from a 480 deg2 strip centered at R.A. 00h on the celestial equator with additional 360 deg2 shallower auxiliary fields at other longitudes. The combination of the deepest available 218 GHz wide-field imaging, our 277 GHz data, and multiband filtering results in the most sensitive wide-field millimeter-wave DSFG selection to date, with rms noise level referenced to 218 GHz reaching below 2 mJy. We have developed new techniques to remove Galactic contamination (including evidence for CO (2−1) line emission) from the extragalactic catalog, yielding a catalog of 321 Galactic sources in addition to the extragalactic catalog. We employ a new flux debiasing method that accounts for the heterogeneous sample selection in the presence of Galactic cuts. We present the spectral properties and source counts of the AGNs and DSFGs. The DSFG spectra depart from the Rayleigh–Jeans regime of an optically thin modified blackbody between 218 and 277 GHz, consistent with optically thick emission or an additional cold dust component. For AGNs with 148 and 218 GHz flux density >50 mJy, we estimate the interyear rms fractional deviation in flux density due to source variability to be 40% with a 0.98 interband correlation coefficient. We provide source counts for AGNs in the range of 8–2870 mJy and for DSFGs in the range of 8–90 mJy. Our DSFG counts probe both the brighter, lensed population and the fainter, unlensed population. At 277 GHz we report the first measurements of source counts at these flux densities, finding an excess above most model count predictions. Finally, we present 30 of the brightest DSFGs that were selected for multifrequency study as candidate high-z lensed systems. [ABSTRACT FROM AUTHOR]

Published
2020
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24. The Atacama Cosmology Telescope: two-season ACTPol spectra and parameters

Author

Louis, Thibaut, primary, Grace, Emily, additional, Hasselfield, Matthew, additional, Lungu, Marius, additional, Maurin, Loïc, additional, Addison, Graeme E., additional, Ade, Peter A. R., additional, Aiola, Simone, additional, Allison, Rupert, additional, Amiri, Mandana, additional, Angile, Elio, additional, Battaglia, Nicholas, additional, Beall, James A., additional, de Bernardis, Francesco, additional, Bond, J Richard, additional, Britton, Joe, additional, Calabrese, Erminia, additional, Cho, Hsiao-mei, additional, Choi, Steve K., additional, Coughlin, Kevin, additional, Crichton, Devin, additional, Crowley, Kevin, additional, Datta, Rahul, additional, Devlin, Mark J., additional, Dicker, Simon R., additional, Dunkley, Joanna, additional, Dünner, Rolando, additional, Ferraro, Simone, additional, Fox, Anna E., additional, Gallardo, Patricio, additional, Gralla, Megan, additional, Halpern, Mark, additional, Henderson, Shawn, additional, Hill, J. Colin, additional, Hilton, Gene C., additional, Hilton, Matt, additional, Hincks, Adam D., additional, Hlozek, Renée, additional, Ho, S.P. Patty, additional, Huang, Zhiqi, additional, Hubmayr, Johannes, additional, Huffenberger, Kevin M., additional, Hughes, John P., additional, Infante, Leopoldo, additional, Irwin, Kent, additional, Kasanda, Simon Muya, additional, Klein, Jeff, additional, Koopman, Brian, additional, Kosowsky, Arthur, additional, Li, Dale, additional, Madhavacheril, Mathew, additional, Marriage, Tobias A., additional, McMahon, Jeff, additional, Menanteau, Felipe, additional, Moodley, Kavilan, additional, Munson, Charles, additional, Naess, Sigurd, additional, Nati, Federico, additional, Newburgh, Laura, additional, Nibarger, John, additional, Niemack, Michael D., additional, Nolta, Michael R., additional, Nuñez, Carolina, additional, Page, Lyman A., additional, Pappas, Christine, additional, Partridge, Bruce, additional, Rojas, Felipe, additional, Schaan, Emmanuel, additional, Schmitt, Benjamin L., additional, Sehgal, Neelima, additional, Sherwin, Blake D., additional, Sievers, Jon, additional, Simon, Sara, additional, Spergel, David N., additional, Staggs, Suzanne T., additional, Switzer, Eric R., additional, Thornton, Robert, additional, Trac, Hy, additional, Treu, Jesse, additional, Tucker, Carole, additional, Engelen, Alexander Van, additional, Ward, Jonathan T., additional, and Wollack, Edward J., additional

Published
2017
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30. The Atacama Cosmology Telescope: CMB polarization at 200 < ℓ < 9000

Author

Naess, Sigurd, primary, Hasselfield, Matthew, additional, McMahon, Jeff, additional, Niemack, Michael D., additional, Addison, Graeme E., additional, Ade, Peter A. R., additional, Allison, Rupert, additional, Amiri, Mandana, additional, Battaglia, Nick, additional, Beall, James A., additional, de Bernardis, Francesco, additional, Bond, J Richard, additional, Britton, Joe, additional, Calabrese, Erminia, additional, Cho, Hsiao-mei, additional, Coughlin, Kevin, additional, Crichton, Devin, additional, Das, Sudeep, additional, Datta, Rahul, additional, Devlin, Mark J., additional, Dicker, Simon R., additional, Dunkley, Joanna, additional, Dünner, Rolando, additional, Fowler, Joseph W., additional, Fox, Anna E., additional, Gallardo, Patricio, additional, Grace, Emily, additional, Gralla, Megan, additional, Hajian, Amir, additional, Halpern, Mark, additional, Henderson, Shawn, additional, Hill, J. Colin, additional, Hilton, Gene C., additional, Hilton, Matt, additional, Hincks, Adam D., additional, Hlozek, Renée, additional, Ho, Patty, additional, Hubmayr, Johannes, additional, Huffenberger, Kevin M., additional, Hughes, John P., additional, Infante, Leopoldo, additional, Irwin, Kent, additional, Jackson, Rebecca, additional, Kasanda, Simon Muya, additional, Klein, Jeff, additional, Koopman, Brian, additional, Kosowsky, Arthur, additional, Li, Dale, additional, Louis, Thibaut, additional, Lungu, Marius, additional, Madhavacheril, Mathew, additional, Marriage, Tobias A., additional, Maurin, Loïc, additional, Menanteau, Felipe, additional, Moodley, Kavilan, additional, Munson, Charles, additional, Newburgh, Laura, additional, Nibarger, John, additional, Nolta, Michael R., additional, Page, Lyman A., additional, Pappas, Christine, additional, Partridge, Bruce, additional, Rojas, Felipe, additional, Schmitt, Benjamin L., additional, Sehgal, Neelima, additional, Sherwin, Blake D., additional, Sievers, Jon, additional, Simon, Sara, additional, Spergel, David N., additional, Staggs, Suzanne T., additional, Switzer, Eric R., additional, Thornton, Robert, additional, Trac, Hy, additional, Tucker, Carole, additional, Uehara, Masao, additional, Engelen, Alexander Van, additional, Ward, Jonathan T., additional, and Wollack, Edward J., additional

Published
2014
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31. Precision epoch of reionization studies with next-generation CMB experiments

Author

Calabrese, Erminia, primary, Hložek, Renée, additional, Battaglia, Nick, additional, Bond, J. Richard, additional, de Bernardis, Francesco, additional, Devlin, Mark J., additional, Hajian, Amir, additional, Henderson, Shawn, additional, Hil, J. Colin, additional, Kosowsky, Arthur, additional, Louis, Thibaut, additional, McMahon, Jeff, additional, Moodley, Kavilan, additional, Newburgh, Laura, additional, Niemack, Michael D., additional, Page, Lyman A., additional, Partridge, Bruce, additional, Sehgal, Neelima, additional, Sievers, Jonathan L., additional, Spergel, David N., additional, Staggs, Suzanne T., additional, Switzer, Eric R., additional, Trac, Hy, additional, and Wollack, Edward J., additional

Published
2014
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32. The Atacama Cosmology Telescope: cross correlation withPlanckmaps

Author

Louis, Thibaut, primary, Addison, Graeme E., additional, Hasselfield, Matthew, additional, Bond, J. Richard, additional, Calabrese, Erminia, additional, Das, Sudeep, additional, Devlin, Mark J., additional, Dunkley, Joanna, additional, Dünner, Rolando, additional, Gralla, Megan, additional, Hajian, Amir, additional, Hincks, Adam D., additional, Hlozek, Renée, additional, Huffenberger, Kevin, additional, Infante, Leopoldo, additional, Kosowsky, Arthur, additional, Marriage, Tobias A., additional, Moodley, Kavilan, additional, Næss, Sigurd, additional, Niemack, Michael D., additional, Nolta, Michael R., additional, Page, Lyman A., additional, Partridge, Bruce, additional, Sehgal, Neelima, additional, Sievers, Jonathan L., additional, Spergel, David N., additional, Staggs, Suzanne T., additional, Walter, Benjamin Z., additional, and Wollack, Edward J., additional

Published
2014
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33. The Atacama Cosmology Telescope: temperature and gravitational lensing power spectrum measurements from three seasons of data

Author

Das, Sudeep, primary, Louis, Thibaut, additional, Nolta, Michael R., additional, Addison, Graeme E., additional, Battistelli, Elia S., additional, Bond, J Richard, additional, Calabrese, Erminia, additional, Crichton, Devin, additional, Devlin, Mark J., additional, Dicker, Simon, additional, Dunkley, Joanna, additional, Dünner, Rolando, additional, Fowler, Joseph W., additional, Gralla, Megan, additional, Hajian, Amir, additional, Halpern, Mark, additional, Hasselfield, Matthew, additional, Hilton, Matt, additional, Hincks, Adam D., additional, Hlozek, Renée, additional, Huffenberger, Kevin M., additional, Hughes, John P., additional, Irwin, Kent D., additional, Kosowsky, Arthur, additional, Lupton, Robert H., additional, Marriage, Tobias A., additional, Marsden, Danica, additional, Menanteau, Felipe, additional, Moodley, Kavilan, additional, Niemack, Michael D., additional, Page, Lyman A., additional, Partridge, Bruce, additional, Reese, Erik D., additional, Schmitt, Benjamin L., additional, Sehgal, Neelima, additional, Sherwin, Blake D., additional, Sievers, Jonathan L., additional, Spergel, David N., additional, Staggs, Suzanne T., additional, Swetz, Daniel S., additional, Switzer, Eric R., additional, Thornton, Robert, additional, Trac, Hy, additional, and Wollack, Ed, additional

Published
2014
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35. The Atacama Cosmology Telescope: cosmological parameters from three seasons of data

Author

Sievers, Jonathan L, primary, Hlozek, Renée A, additional, Nolta, Michael R, additional, Acquaviva, Viviana, additional, Addison, Graeme E, additional, Ade, Peter A. R, additional, Aguirre, Paula, additional, Amiri, Mandana, additional, Appel, John William, additional, Barrientos, L. Felipe, additional, Battistelli, Elia S, additional, Battaglia, Nick, additional, Bond, J. Richard, additional, Brown, Ben, additional, Burger, Bryce, additional, Calabrese, Erminia, additional, Chervenak, Jay, additional, Crichton, Devin, additional, Das, Sudeep, additional, Devlin, Mark J, additional, Dicker, Simon R, additional, Doriese, W. Bertrand, additional, Dunkley, Joanna, additional, Dünner, Rolando, additional, Essinger-Hileman, Thomas, additional, Faber, David, additional, Fisher, Ryan P, additional, Fowler, Joseph W, additional, Gallardo, Patricio, additional, Gordon, Michael S, additional, Gralla, Megan B, additional, Hajian, Amir, additional, Halpern, Mark, additional, Hasselfield, Matthew, additional, Hernández-Monteagudo, Carlos, additional, Hill, J. Colin, additional, Hilton, Gene C, additional, Hilton, Matt, additional, Hincks, Adam D, additional, Holtz, Dave, additional, Huffenberger, Kevin M, additional, Hughes, David H, additional, Hughes, John P, additional, Infante, Leopoldo, additional, Irwin, Kent D, additional, Jacobson, David R, additional, Johnstone, Brittany, additional, Juin, Jean Baptiste, additional, Kaul, Madhuri, additional, Klein, Jeff, additional, Kosowsky, Arthur, additional, Lau, Judy M, additional, Limon, Michele, additional, Lin, Yen-Ting, additional, Louis, Thibaut, additional, Lupton, Robert H, additional, Marriage, Tobias A, additional, Marsden, Danica, additional, Martocci, Krista, additional, Mauskopf, Phil, additional, McLaren, Michael, additional, Menanteau, Felipe, additional, Moodley, Kavilan, additional, Moseley, Harvey, additional, Netterfield, Calvin B, additional, Niemack, Michael D, additional, Page, Lyman A, additional, Page, William A, additional, Parker, Lucas, additional, Partridge, Bruce, additional, Plimpton, Reed, additional, Quintana, Hernan, additional, Reese, Erik D, additional, Reid, Beth, additional, Rojas, Felipe, additional, Sehgal, Neelima, additional, Sherwin, Blake D, additional, Schmitt, Benjamin L, additional, Spergel, David N, additional, Staggs, Suzanne T, additional, Stryzak, Omelan, additional, Swetz, Daniel S, additional, Switzer, Eric R, additional, Thornton, Robert, additional, Trac, Hy, additional, Tucker, Carole, additional, Uehara, Masao, additional, Visnjic, Katerina, additional, Warne, Ryan, additional, Wilson, Grant, additional, Wollack, Ed, additional, Zhao, Yue, additional, and Zunckel, Caroline, additional

Published
2013
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36. The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy clusters at 148 GHz from three seasons of data

Author

Hasselfield, Matthew, primary, Hilton, Matt, additional, Marriage, Tobias A, additional, Addison, Graeme E, additional, Barrientos, L. Felipe, additional, Battaglia, Nicholas, additional, Battistelli, Elia S, additional, Bond, J. Richard, additional, Crichton, Devin, additional, Das, Sudeep, additional, Devlin, Mark J, additional, Dicker, Simon R, additional, Dunkley, Joanna, additional, Dünner, Rolando, additional, Fowler, Joseph W, additional, Gralla, Megan B, additional, Hajian, Amir, additional, Halpern, Mark, additional, Hincks, Adam D, additional, Hlozek, Renée, additional, Hughes, John P, additional, Infante, Leopoldo, additional, Irwin, Kent D, additional, Kosowsky, Arthur, additional, Marsden, Danica, additional, Menanteau, Felipe, additional, Moodley, Kavilan, additional, Niemack, Michael D, additional, Nolta, Michael R, additional, Page, Lyman A, additional, Partridge, Bruce, additional, Reese, Erik D, additional, Schmitt, Benjamin L, additional, Sehgal, Neelima, additional, Sherwin, Blake D, additional, Sievers, Jon, additional, Sifón, Cristóbal, additional, Spergel, David N, additional, Staggs, Suzanne T, additional, Swetz, Daniel S, additional, Switzer, Eric R, additional, Thornton, Robert, additional, Trac, Hy, additional, and Wollack, Edward J, additional

Published
2013
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43. ON THE CLUSTER PHYSICS OF SUNYAEV-ZEL'DOVICH AND X-RAY SURVEYS. III. MEASUREMENT BIASES AND COSMOLOGICAL EVOLUTION OF GAS AND STELLAR MASS FRACTIONS.

Author

Battaglia, N., Bond, J. R., Pfrommer, C., and Sievers, J. L.

Subjects
*METAPHYSICAL cosmology, *GALAXY clusters, *PHYSICS, *DARK matter, *BARYONS
Abstract

Gas masses tightly correlate with the virial masses of galaxy clusters, allowing for a precise determination of cosmological parameters by means of X-ray surveys. However, the gas mass fractions (fgas) at the virial radius (R200) derived from recent Suzaku observations are considerably larger than the cosmic mean, calling into question the accuracy of cosmological parameters. Here, we use a large suite of cosmological hydrodynamical simulations to study measurement biases of fgas. We employ different variants of simulated physics, including radiative gas physics, star formation, and thermal feedback by active galactic nuclei, which we show is able to arrest overcooling and to result in constant stellar mass fractions for redshifts z < 1. Computing the mass profiles in 48 angular cones, we find anisotropic gas and total mass distributions that imply an angular variance of fgas at the level of 30%. This anisotropy originates from the recent formation epoch of clusters and from the strong internal baryon-to-dark-matter density bias. In the most extreme cones, fgas can be biased high by a factor of two at R200 in massive clusters (M200 ∼ 1015M☼), thereby providing an explanation for high fgas measurements by Suzaku. While projection lowers this factor, there are other measurement biases that may (partially) compensate. At R200, fgas is biased high by 20% when assuming hydrostatic equilibrium masses, i.e., neglecting the kinetic pressure, and by another ∼10%-20% due to the presence of density clumping. At larger radii, both measurement biases increase dramatically. While the cluster sample variance of the true fgas decreases to a level of 5% at R200, the sample variance that includes both measurement biases remains fairly constant at the level of 10%-20%. The constant redshift evolution of fgas within R500 for massive clusters is encouraging for using gas masses to derive cosmological parameters, provided the measurement biases can be controlled. [ABSTRACT FROM AUTHOR]

Published
2013
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44. THE ATACAMA COSMOLOGY TELESCOPE: BEAM MEASUREMENTS AND THE MICROWAVE BRIGHTNESS TEMPERATURES OF URANUS AND SATURN.

Author

Hasselfield, Matthew, Moodley, Kavilan, Bond, J. Richard, Das, Sudeep, Devlin, Mark J., Dunkley, Joanna, Dünner, Rolando, Fowler, Joseph W., Gallardo, Patricio, Gralla, Megan B., Hajian, Amir, Halpern, Mark, Hincks, Adam D., Marriage, Tobias A., Marsden, Danica, Niemack, Michael D., Nolta, Michael R., Page, Lyman A., Partridge, Bruce, and Schmitt, Benjamin L.

Published
2013
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45. THE ATACAMA COSMOLOGY TELESCOPE: DYNAMICAL MASSES AND SCALING RELATIONS FOR A SAMPLE OF MASSIVE SUNYAEV-ZEL'DOVICH EFFECT SELECTED GALAXY CLUSTERS.

Author

SIFÓN, CRISTÓBAL, MENANTEAU, FELIPE, HASSELFIELD, MATTHEW, MARRIAGE, TOBIAS A., HUGHES, JOHN P., BARRIENTOS, L. FELIPE, GONZÁLEZ, JORGE, INFANTE, LEOPOLDO, ADDISON, GRAEME E., BAKER, ANDREW J., BATTAGLIA, NICK, BOND, J. RICHARD, CRICHTON, DEVIN, DAS, SUDEEP, DEVLIN, MARK J., DUNKLEY, JOANNA, DÜNNER, ROLANDO, GRALLA, MEGAN B., HAJIAN, AMIR, and HILTON, MATT

Subjects
ARITHMETIC mean, ATACAMENO language, METAPHYSICAL cosmology, GALAXY clusters, STANDARD deviations
Abstract

We present the first dynamical mass estimates and scaling relations for a sample of Sunyaev-Zel'dovich effect (SZE) selected galaxy clusters. The sample consists of 16 massive clusters detected with the Atacama Cosmology Telescope (ACT) over a 455 deg2 area of the southern sky. Deep multi-object spectroscopic observations were taken to secure intermediate-resolution (R ~ 700-800) spectra and redshifts for ≈60 member galaxies on average per cluster. The dynamical masses M200c of the clusters have been calculated using simulation-based scaling relations between velocity dispersion and mass. The sample has a median redshift z = 0.50 and a median mass M200c ☉ 12 × 1014 h -1 70 M☉ with a lower limit M200c ≃ 6 × 1014 h -1 70 M☉, consistent with the expectations for the ACT southern sky survey. These masses are compared to the ACT SZE properties of the sample, specifically, the match-filtered central SZE amplitude ~y0, the central Compton parameter ~y0, and the integrated Compton signal Y200c, which we use to derive SZE-mass scaling relations. All SZE estimators correlate with dynamical mass with low intrinsic scatter (≲20%), in agreement with numerical simulations. We explore the effects of various systematic effects on these scaling relations, including the correlation between observables and the influence of dynamically disturbed clusters. Using the three-dimensional information available, we divide the sample into relaxed and disturbed clusters and find that ~50% of the clusters are disturbed. There are hints that disturbed systems might bias the scaling relations, but given the current sample sizes, these differences are not significant; further studies including more clusters are required to assess the impact of these clusters on the scaling relations. [ABSTRACT FROM AUTHOR]

Published
2013
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46. PRIMORDIAL GRAVITATIONAL WAVE DETECTABILITY WITH DEEP SMALL-SKY COSMIC MICROWAVE BACKGROUND EXPERIMENTS.

Author

FARHANG, M., BOND, J. R., DORé, O., and NETTERFIELD, C. B.

Subjects
*GRAVITATIONAL waves, *GRAVITATIONAL wave detectors, *COSMIC background radiation, *BAYES' estimation, *PLANCK (Artificial satellite), *COSMOLOGICAL principle
Abstract

We use the Bayesian estimation on direct T -Q-U cosmic microwave background (CMB) polarization maps to forecast errors on the tensor-to-scalar power ratio r, and hence on primordial gravitational waves, as a function of sky coverage fsky. This map-based likelihood filters the information in the pixel-pixel space into the optimal combinations needed for r detection for cut skies, providing enhanced information over a first-step linear separation into a combination of E, B, and mixed modes, and ignoring the latter. With current computational power and for typical resolutions appropriate for r detection, the large matrix inversions required are accurate and fast. Our simulations explore two classes of experiments, with differing bolometric detector numbers, sensitivities, and observational strategies. One is motivated by a long duration balloon experiment like Spider, with pixel noise α √ fsky for a specified observing period. This analysis also applies to ground-based array experiments. We find that, in the absence of systematic effects and foregrounds, an experiment with Spider-like noise concentrating on fsky ~ 0.02-0.2 could place a 2σr ≈ 0.014 boundary (~95% confidence level), which rises to 0.02 with an ⨏-dependent foreground residual left over from an assumed efficient component separation. We contrast this with a Planck-like fixed instrumental noise as fsky varies, which gives a Galaxy-masked (fsky = 0.75) 2σr ≈ 0.015, rising to ≈0.05 with the foreground residuals. Using as the figure of merit the (marginalized) one-dimensional Shannon entropy of r, taken relative to the first 2003 WMAP CMB-only constraint, gives -2.7 bits from the 2012 WMAP9+ACT+SPT+LSS data, and forecasts of -6 bits from Spider (+ Planck); this compares with up to -11 bits for CMBPol, COrE, and PIXIE post-Planck satellites and -13 bits for a perfectly noiseless cosmic variance limited experiment. We thus confirm the wisdom of the current strategy for r detection of deeply probed patches covering the fsky minimum-error trough with balloon and ground experiments. [ABSTRACT FROM AUTHOR]

Published
2013
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48. The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy clusters at 148GHz from three seasons of data.

Author

Hasselfield, Matthew, Hilton, Matt, Marriage, Tobias A., Addison, Graeme E., Barrientos, L. Felipe, Battaglia, Nicholas, Battistelli, Elia S., Bond, J. Richard, Crichton, Devin, Das, Sudeep, Devlin, Mark J., Dicker, Simon R., Dunkley, Joanna, Dünner, Rolando, Fowler, Joseph W., Gralla, Megan B., Hajian, Amir, Halpern, Mark, Hincks, Adam D., and Hlozek, Renée

Published
2013
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49. THE ATACAMA COSMOLOGY TELESCOPE: RELATION BETWEEN GALAXY CLUSTER OPTICAL RICHNESS AND SUNYAEV-ZEL'DOVICH EFFECT.

Author

SEHGAL, NEELIMA, ADDISON, GRAEME, BATTAGLIA, NICK, BATTISTELLI, ELIA S., RICHARD BOND, J., DAS, SUDEEP, DEVLIN, MARK J., DUNKLEY, JOANNA, DÜNNER, ROLANDO, GRALLA, MEGAN, HAJIAN, AMIR, HALPERN, MARK, HASSELFIELD, MATTHEW, HILTON, MATT, HINCKS, ADAM D., HLOZEK, RENÉE, HUGHES, JOHN P., KOSOWSKY, ARTHUR, LIN, YEN-TING, and LOUIS, THIBAUT

Subjects
METAPHYSICAL cosmology, LARGE astronomical telescopes, EQUATORIAL satellites, GALAXY clusters, PLANCK (Artificial satellite), STELLAR mass
Abstract

We present the measured Sunyaev-Zel'dovich (SZ) flux from 474 optically selected MaxBCG clusters that fall within the Atacama Cosmology Telescope (ACT) Equatorial survey region. The ACT Equatorial region used in this analysis covers 510 deg2 and overlaps Stripe 82 of the Sloan Digital Sky Survey.We also present the measured SZ flux stacked on 52 X-ray-selected MCXC clusters that fall within the ACT Equatorial region and an ACT Southern survey region covering 455 deg2. We find that the measured SZ flux from the X-ray-selected clusters is consistent with expectations. However, we find that the measured SZ flux from the optically selected clusters is both significantly lower than expectations and lower than the recovered SZ flux measured by the Planck satellite. Since we find a lower recovered SZ signal than Planck, we investigate the possibility that there is a significant offset between the optically selected brightest cluster galaxies (BCGs) and the SZ centers, to which ACT is more sensitive due to its finer resolution. Such offsets can arise due to either an intrinsic physical separation between the BCG and the center of the gas concentration or from misidentification of the cluster BCG. We find that the entire discrepancy for both ACT and Planck can be explained by assuming that the BCGs are offset from the SZ maxima with a uniform random distribution between 0 and 1.5 Mpc. Such large offsets between gas peaks and BCGs for optically selected cluster samples seem unlikely given that we find the physical separation between BCGs and X-ray peaks for an X-ray-selected subsample of MaxBCG clusters to have a much narrower distribution that peaks within 0.2 Mpc. It is possible that other effects are lowering the ACT and Planck signals by the same amount, with offsets between BCGs and SZ peaks explaining the remaining difference between ACT and Planck measurements. Several effects that can lower the SZ signal equally for both ACT and Planck, but not explain the difference in measured signals, include a larger percentage of false detections in the MaxBCG sample, a lower normalization of the mass-richness relation, radio or infrared galaxy contamination of the SZ flux, and a low intrinsic SZ signal. In the latter two cases, the effects would need to be preferentially more significant in the optically selected MaxBCG sample than in the MCXC X-ray sample. [ABSTRACT FROM AUTHOR]

Published
2013
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50. THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE PRIMORDIAL POWER SPECTRUM.

Author

HLOZEK, RENÉE, DUNKLEY, JOANNA, ADDISON, GRAEME, APPEL, JOHN WILLIAM, BOND, J. RICHARD, CARVALHO, C. SOFIA, DAS, SUDEEP, DEVLIN, MARK J., DÜNNER, ROLANDO, ESSINGER-HILEMAN, THOMAS, FOWLER, JOSEPH W., GALLARDO, PATRICIO, HAJIAN, AMIR, HALPERN, MARK, HASSELFIELD, MATTHEW, HILTON, MATT, HINCKS, ADAM D., HUGHES, JOHN P., IRWIN, KENT D., and KLEIN, JEFF

Subjects
COSMIC background radiation, METAPHYSICAL cosmology, ASTRONOMICAL perturbation, GALAXIES
Abstract

We present constraints on the primordial power spectrum of adiabatic fluctuations using data from the 2008 Southern Survey of the Atacama Cosmology Telescope (ACT) in combination with measurements from the Wilkinson Microwave Anisotropy Probe and a prior on the Hubble constant. The angular resolution of ACT provides sensitivity to scales beyond l = 1000 for resolution of multiple peaks in the primordial temperature power spectrum, which enables us to probe the primordial power spectrum of adiabatic scalar perturbations with wavenumbers up to k ≃ 0.2Mpc-1. We find no evidence for deviation from power-law fluctuations over two decades in scale. Matter fluctuations inferred from the primordial temperature power spectrum evolve over cosmic time and can be used to predict the matter power spectrum at late times; we illustrate the overlap of the matter power inferred from cosmic microwave background measurements (which probe the power spectrum in the linear regime) with existing probes of galaxy clustering, cluster abundances, and weak-lensing constraints on the primordial power. This highlights the range of scales probed by current measurements of the matter power spectrum. [ABSTRACT FROM AUTHOR]

Published
2012
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