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41 results on '"Newburgh L. B."'

1. MERGHERS Pilot: MeerKAT discovery of diffuse emission in nine massive Sunyaev-Zel'dovich-selected galaxy clusters from ACT

Author: Knowles, K., Pillay, D. S., Amodeo, S., Baker, A. J., Basu, K., Crichton, D., de Gasperin, F., Devlin, M., Ferrari, C., Hilton, M., Huffenberger, K. M., Hughes, J. P., Koopman, B. J., Moodley, K., Mroczkowski, T., Naess, S., Nati, F., Newburgh, L. B., Oozeer, N., Page, L., Partridge, B., Pfrommer, C., Salatino, M., Schillaci, A., Sifón, C., Smirnov, O., Sikhosana, S. P., Wollack, E. J., and Xu, Z.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The MeerKAT Exploration of Relics, Giant Halos, and Extragalactic Radio Sources (MERGHERS) survey is a planned project to study a large statistical sample of galaxy clusters with the MeerKAT observatory. Here we present the results of a 16--hour pilot project, observed in response to the 2019 MeerKAT Shared Risk proposal call, to test the feasibility of using MeerKAT for a large cluster study using short (0.2--2.1\,hour) integration times. The pilot focuses on 1.28\,GHz observations of 13 massive, low-to-intermediate redshift ($0.22 < z < 0.65$) clusters from the Sunyaev-Zel'dovich-selected Atacama Cosmology Telescope (ACT) DR5 catalogue that show multiwavelength indications of dynamical disturbance. With a 70 per cent detection rate (9/13 clusters), this pilot study validates our proposed MERGHERS observing strategy and provides twelve detections of diffuse emission, eleven of them new, indicating the strength of MeerKAT for such types of studies. The detections (signal-to-noise ratio $\gtrsim6$) are summarised as follows: two systems host both relic(s) and a giant radio halo, five systems host radio halos, and two have candidate radio halos. Power values, $k$-corrected to 1.4 GHz assuming a fiducial spectral index of $\alpha = -1.3 \pm 0.4$, are consistent with known radio halo and relic scaling relations., Comment: 9 pages, 4 figures, 2 tables. Accepted to MNRAS
Published: 2020
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2. The Atacama Cosmology Telescope: A Catalog of > 4000 Sunyaev-Zel'dovich Galaxy Clusters

Author: Hilton, M., Sifón, C., Naess, S., Madhavacheril, M., Oguri, M., Rozo, E., Rykoff, E., Abbott, T. M. C., Adhikari, S., Aguena, M., Aiola, S., Allam, S., Amodeo, S., Amon, A., Annis, J., Ansarinejad, B., Aros-Bunster, C., Austermann, J. E., Avila, S., Bacon, D., Battaglia, N., Beall, J. A., Becker, D. T., Bernstein, G. M., Bertin, E., Bhandarkar, T., Bhargava, S., Bond, J. R., Brooks, D., Burke, D. L., Calabrese, E., Carretero, J., Choi, S. K., Choi, A., Conselice, C., da Costa, L. N., Costanzi, M., Crichton, D., Crowley, K. T., Dünner, R., Denison, E. V., Devlin, M. J., Dicker, S. R., Diehl, H. T., Dietrich, J. P., Doel, P., Duff, S. M., Duivenvoorden, A. J., Dunkley, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giles, P., Golec, J. E., Gralla, M. B., Grandis, S., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Han, D., Hartley, W. G., Hasselfield, M., Hill, J. C., Hilton, G. C., Hincks, A. D., Hinton, S. R., Ho, S-P. P., Honscheid, K., Hoyle, B., Hubmayr, J., Huffenberger, K. M., Hughes, J. P., Jaelani, A. T., Jain, B., James, D. J., Jeltema, T., Kent, S., Kind, M. Carrasco, Knowles, K., Koopman, B. J., Kuehn, K., Lahav, O., Lima, M., Lin, Y-T., Lokken, M., Loubser, S. I., MacCrann, N., Maia, M. A. G., Marriage, T. A., Martin, J., McMahon, J., Melchior, P., Menanteau, F., Miquel, R., Miyatake, H., Moodley, K., Morgan, R., Mroczkowski, T., Nati, F., Newburgh, L. B., Niemack, M. D., Nishizawa, A. J., Ogando, R. L. C., Orlowski-Scherer, J., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Phakathi, P., Plazas, A. A., Robertson, N. C., Romer, A. K., Rosell, A. Carnero, Salatino, M., Sanchez, E., Schaan, E., Schillaci, A., Sehgal, N., Serrano, S., Shin, T., Simon, S. M., Smith, M., Soares-Santos, M., Spergel, D. N., Staggs, S. T., Storer, E. R., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Trac, H., Ullom, J. N., Vale, L. R., Van Lanen, J., Vavagiakis, E. M., De Vicente, J., Wilkinson, R. D., Wollack, E. J., Xu, Z., and Zhang, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a catalog of 4195 optically confirmed Sunyaev-Zel'dovich (SZ) selected galaxy clusters detected with signal-to-noise > 4 in 13,211 deg$^2$ of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multi-frequency matched filter to 98 and 150 GHz maps constructed from ACT observations obtained from 2008-2018, and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04 < z < 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ-signal vs. mass scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M500c > 3.8 x 10$^{14}$ MSun, evaluated at z = 0.5, for clusters detected at signal-to-noise ratio > 5 in maps filtered at an angular scale of 2.4'. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ-signal mass-scaling relation, such as the Dark Energy Survey (4566 deg$^2$), the Hyper Suprime-Cam Subaru Strategic Program (469 deg$^2$), and the Kilo Degree Survey (825 deg$^2$). We highlight some noteworthy objects in the sample, including potentially projected systems; clusters with strong lensing features; clusters with active central galaxies or star formation; and systems of multiple clusters that may be physically associated. The cluster catalog will be a useful resource for future cosmological analyses, and studying the evolution of the intracluster medium and galaxies in massive clusters over the past 10 Gyr., Comment: 35 pages, 27 figures, accepted for publication in ApJS; v1.0 catalogs will be available from LAMBDA https://lambda.gsfc.nasa.gov/product/act/actpol_prod_table.cfm; v1.0 catalogs available from https://astro.ukzn.ac.za/~mjh/ACTDR5/v1.0/ until then
Published: 2020
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3. A bright millisecond-duration radio burst from a Galactic magnetar

Author: Collaboration, The CHIME/FRB, Andersen, B. C., Bandura, K. M., Bhardwaj, M., Bij, A., Boyce, M. M., Boyle, P. J., Brar, C., Cassanelli, T., Chawla, P., Chen, T., Cliche, J. -F., Cook, A., Cubranic, D., Curtin, A. P., Denman, N. T., Dobbs, M., Dong, F. Q., Fandino, M., Fonseca, E., Gaensler, B. M., Giri, U., Good, D. C., Halpern, M., Hill, A. S., Hinshaw, G. F., Höfer, C., Josephy, A., Kania, J. W., Kaspi, V. M., Landecker, T. L., Leung, C., Li, D. Z., Lin, H. -H., Masui, K. W., Mckinven, R., Mena-Parra, J., Merryfield, M., Meyers, B. W., Michilli, D., Milutinovic, N., Mirhosseini, A., Münchmeyer, M., Naidu, A., Newburgh, L. B., Ng, C., Patel, C., Pen, U. -L., Pinsonneault-Marotte, T., Pleunis, Z., Quine, B. M., Rafiei-Ravandi, M., Rahman, M., Ransom, S. M., Renard, A., Sanghavi, P., Scholz, P., Shaw, J. R., Shin, K., Siegel, S. R., Singh, S., Smegal, R. J., Smith, K. M., Stairs, I. H., Tan, C. M., Tendulkar, S. P., Tretyakov, I., Vanderlinde, K., Wang, H., Wulf, D., and Zwaniga, A. V.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Magnetars are highly magnetized young neutron stars that occasionally produce enormous bursts and flares of X-rays and gamma-rays. Of the approximately thirty magnetars currently known in our Galaxy and Magellanic Clouds, five have exhibited transient radio pulsations. Fast radio bursts (FRBs) are millisecond-duration bursts of radio waves arriving from cosmological distances. Some have been seen to repeat. A leading model for repeating FRBs is that they are extragalactic magnetars, powered by their intense magnetic fields. However, a challenge to this model has been that FRBs must have radio luminosities many orders of magnitude larger than those seen from known Galactic magnetars. Here we report the detection of an extremely intense radio burst from the Galactic magnetar SGR 1935+2154 using the Canadian Hydrogen Intensity Mapping Experiment (CHIME) FRB project. The fluence of this two-component bright radio burst and the estimated distance to SGR 1935+2154 together imply a 400-800 MHz burst energy of $\sim 3 \times 10^{34}$ erg, which is three orders of magnitude brighter than those of any radio-emitting magnetar detected thus far. Such a burst coming from a nearby galaxy would be indistinguishable from a typical FRB. This event thus bridges a large fraction of the radio energy gap between the population of Galactic magnetars and FRBs, strongly supporting the notion that magnetars are the origin of at least some FRBs., Comment: Submitted to Nature. This version: Geocentric arrival time corrected
Published: 2020
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4. Periodic activity from a fast radio burst source

Author: Collaboration, The CHIME/FRB, Amiri, M., Andersen, B. C., Bandura, K. M., Bhardwaj, M., Boyle, P. J., Brar, C., Chawla, P., Chen, T., Cliche, J. F., Cubranic, D., Deng, M., Denman, N. T., Dobbs, M., Dong, F. Q., Fandino, M., Fonseca, E., Gaensler, B. M., Giri, U., Good, D. C., Halpern, M., Hessels, J. W. T., Hill, A. S., Höfer, C., Josephy, A., Kania, J. W., Karuppusamy, R., Kaspi, V. M., Keimpema, A., Kirsten, F., Landecker, T. L., Lang, D. A., Leung, C., Li, D. Z., Lin, H. -H., Marcote, B., Masui, K. W., Mckinven, R., Mena-Parra, J., Merryfield, M., Michilli, D., Milutinovic, N., Mirhosseini, A., Naidu, A., Newburgh, L. B., Ng, C., Nimmo, K., Paragi, Z., Patel, C., Pen, U. -L., Pinsonneault-Marotte, T., Pleunis, Z., Rafiei-Ravandi, M., Rahman, M., Ransom, S. M., Renard, A., Sanghavi, P., Scholz, P., Shaw, J. R., Shin, K., Siegel, S. R., Singh, S., Smegal, R. J., Smith, K. M., Stairs, I. H., Tendulkar, S. P., Tretyakov, I., Vanderlinde, K., Wang, H., Wang, X., Wulf, D., Yadav, P., and Zwaniga, A. V.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Fast radio bursts (FRBs) are bright, millisecond-duration radio transients originating from extragalactic distances. Their origin is unknown. Some FRB sources emit repeat bursts, ruling out cataclysmic origins for those events. Despite searches for periodicity in repeat burst arrival times on time scales from milliseconds to many days, these bursts have hitherto been observed to appear sporadically, and though clustered, without a regular pattern. Here we report the detection of a $16.35\pm0.15$ day periodicity (or possibly a higher-frequency alias of that periodicity) from a repeating FRB 180916.J0158+65 detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project (CHIME/FRB). In 38 bursts recorded from September 16th, 2018 through February 4th, 2020, we find that all bursts arrive in a 5-day phase window, and 50% of the bursts arrive in a 0.6-day phase window. Our results suggest a mechanism for periodic modulation either of the burst emission itself, or through external amplification or absorption, and disfavour models invoking purely sporadic processes.
Published: 2020
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5. CHIME/FRB Detection of Eight New Repeating Fast Radio Burst Sources

Author: Collaboration, The CHIME/FRB, Andersen, B. C., Bandura, K., Bhardwaj, M., Boubel, P., Boyce, M. M., Boyle, P. J., Brar, C., Cassanelli, T., Chawla, P., Cubranic, D., Deng, M., Dobbs, M., Fandino, M., Fonseca, E., Gaensler, B. M., Gilbert, A. J., Giri, U., Good, D. C., Halpern, M., Hill, A. S., Hinshaw, G., Höfer, C., Josephy, A., Kaspi, V. M., Kothes, R., Landecker, T. L., Lang, D. A., Li, D. Z., Lin, H. -H., Masui, K. W., Mena-Parra, J., Merryfield, M., Mckinven, R., Michilli, D., Milutinovic, N., Naidu, A., Newburgh, L. B., Ng, C., Patel, C., Pen, U., Pinsonneault-Marotte, T., Pleunis, Z., Rafiei-Ravandi, M., Rahman, M., Ransom, S. M., Renard, A., Scholz, P., Siegel, S. R., Singh, S., Smith, K. M., Stairs, I. H., Tendulkar, S. P., Tretyakov, I., Vanderlinde, K., Yadav, P., and Zwaniga, A. V.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the discovery of eight repeating fast radio burst (FRB) sources found using the Canadian Hydrogen Intensity Mapping Experiment (CHIME) telescope. These sources span a dispersion measure (DM) range of 103.5 to 1281 pc cm$^{-3}$. They display varying degrees of activity: six sources were detected twice, another three times, and one ten times. These eight repeating FRBs likely represent the bright and/or high-rate end of a distribution of infrequently repeating sources. For all sources, we determine sky coordinates with uncertainties of $\sim$10$^\prime$. FRB 180916.J0158+65 has a burst-averaged DM = $349.2 \pm 0.3$ pc cm$^{-3}$ and a low DM excess over the modelled Galactic maximum (as low as $\sim$20 pc cm$^{-3}$); this source also has a Faraday rotation measure (RM) of $-114.6 \pm 0.6$ rad m$^{-2}$, much lower than the RM measured for FRB 121102. FRB 181030.J1054+73 has the lowest DM for a repeater, $103.5 \pm 0.3$ pc cm$^{-3}$, with a DM excess of $\sim$ 70 pc cm$^{-3}$. Both sources are interesting targets for multi-wavelength follow-up due to their apparent proximity. The DM distribution of our repeater sample is statistically indistinguishable from that of the first 12 CHIME/FRB sources that have not repeated. We find, with 4$\sigma$ significance, that repeater bursts are generally wider than those of CHIME/FRB bursts that have not repeated, suggesting different emission mechanisms. Our repeater events show complex morphologies that are reminiscent of the first two discovered repeating FRBs. The repetitive behavior of these sources will enable interferometric localizations and subsequent host galaxy identifications., Comment: 40 pages, 11 figures; accepted by ApJL on 28 September 2019; added analysis of correlation between width and max. flux density
Published: 2019
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6. A Second Source of Repeating Fast Radio Bursts

Author: Collaboration, The CHIME/FRB, Amiri, M., Bandura, K., Bhardwaj, M., Boubel, P., Boyce, M. M., Boyle, P. J., Brar, C., Burhanpurkar, M., Cassanelli, T., Chawla, P., Cliche, J. F., Cubranic, D., Deng, M., Denman, N., Dobbs, M., Fandino, M., Fonseca, E., Gaensler, B. M., Gilbert, A. J., Gill, A., Giri, U., Good, D. C., Halpern, M., Hanna, D. S., Hill, A. S., Hinshaw, G., Höfer, C., Josephy, A., Kaspi, V. M., Landecker, T. L., Lang, D. A., Lin, H. -H., Masui, K. W., Mckinven, R., Mena-Parra, J., Merryfield, M., Michilli, D., Milutinovic, N., Moatti, C., Naidu, A., Newburgh, L. B., Ng, C., Patel, C., Pen, U. -L., Pinsonneault-Marotte, T., Pleunis, Z., Rafiei-Ravandi, M., Rahman, M., Ransom, S. M., Renard, A., Scholz, P., Shaw, J. R., Siegel, S. R., Smith, K. M., Stairs, I. H., Tendulkar, S. P., Tretyakov, I., Vanderlinde, K., and Yadav, P.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The discovery of a repeating Fast Radio Burst (FRB) source, FRB 121102, eliminated models involving cataclysmic events for this source. No other repeating FRB has yet been detected in spite of many recent FRB discoveries and follow-ups, suggesting repeaters may be rare in the FRB population. Here we report the detection of six repeat bursts from FRB 180814.J0422+73, one of the 13 FRBs detected by the Canadian Hydrogen Intensity Mapping Experiment (CHIME) FRB project during its pre-commissioning phase in July and August 2018. These repeat bursts are consistent with originating from a single position on the sky, with the same dispersion measure (DM), ~189 pc cm-3. This DM is approximately twice the expected Milky Way column density, and implies an upper limit on the source redshift of 0.1, at least a factor of ~2 closer than FRB 121102. In some of the repeat bursts, we observe sub-pulse frequency structure, drifting, and spectral variation reminiscent of that seen in FRB 121102, suggesting similar emission mechanisms and/or propagation effects. This second repeater, found among the first few CHIME/FRB discoveries, suggests that there exists -- and that CHIME/FRB and other wide-field, sensitive radio telescopes will find -- a substantial population of repeating FRBs., Comment: accepted by Nature
Published: 2019
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7. The CHIME Fast Radio Burst Project: System Overview

Author: Collaboration, The CHIME/FRB, Amiri, M., Bandura, K., Berger, P., Bhardwaj, M., Boyce, M. M., Boyle, P. J., Brar, C., Burhanpurkar, M., Chawla, P., Chowdhury, J., Cliche, J. F., Cranmer, M. D., Cubranic, D., Deng, M., Denman, N., Dobbs, M., Fandino, M., Fonseca, E., Gaensler, B. M., Giri, U., Gilbert, A. J., Good, D. C., Guliani, S., Halpern, M., Hinshaw, G., Hofer, C., Josephy, A., Kaspi, V. M., Landecker, T. L., Lang, D., Liao, H., Masui, K. W., Mena-Parra, J., Naidu, A., Newburgh, L. B., Ng, C., Patel, C., Pen, U. -L, Pinsonneault-Marotte, T., Pleunis, Z., Ravandi, M. Rafiei, Ransom, S. M., Renard, A., Scholz, P., Sigurdson, K, Siegel, S. R., Smith, K. M., Stairs, I. H., Tendulkar, S. P., Vanderlinde, K., and Wiebe, D. V.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is a novel transit radio telescope operating across the 400-800-MHz band. CHIME is comprised of four 20-m x 100-m semi-cylindrical paraboloid reflectors, each of which has 256 dual-polarization feeds suspended along its axis, giving it a >200 square degree field-of-view. This, combined with wide bandwidth, high sensitivity, and a powerful correlator makes CHIME an excellent instrument for the detection of Fast Radio Bursts (FRBs). The CHIME Fast Radio Burst Project (CHIME/FRB) will search beam-formed, high time-and frequency-resolution data in real time for FRBs in the CHIME field-of-view. Here we describe the CHIME/FRB backend, including the real-time FRB search and detection software pipeline as well as the planned offline analyses. We estimate a CHIME/FRB detection rate of 2-42 FRBs/sky/day normalizing to the rate estimated at 1.4-GHz by Vander Wiel et al. (2016). Likely science outcomes of CHIME/FRB are also discussed. CHIME/FRB is currently operational in a commissioning phase, with science operations expected to commence in the latter half of 2018., Comment: 27 pages, submitted to ApJ
Published: 2018
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8. HIRAX: A Probe of Dark Energy and Radio Transients

Author: Newburgh, L. B., Bandura, K., Bucher, M. A., Chang, T. -C., Chiang, H. C., Cliche, J. F., Dave, R., Dobbs, M., Clarkson, C., Ganga, K. M., Gogo, T., Gumba, A., Gupta, N., Hilton, M., Johnstone, B., Karastergiou, A., Kunz, M., Lokhorst, D., Maartens, R., Macpherson, S., Mdlalose, M., Moodley, K., Ngwenya, L., Parra, J. M., Peterson, J., Recnik, O., Saliwanchik, B., Santos, M. G., Sievers, J. L., Smirnov, O., Stronkhorst, P., Taylor, R., Vanderlinde, K., Van Vuuren, G., Weltman, A., and Witzemann, A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX) is a new 400-800MHz radio interferometer under development for deployment in South Africa. HIRAX will comprise 1024 six meter parabolic dishes on a compact grid and will map most of the southern sky over the course of four years. HIRAX has two primary science goals: to constrain Dark Energy and measure structure at high redshift, and to study radio transients and pulsars. HIRAX will observe unresolved sources of neutral hydrogen via their redshifted 21-cm emission line (`hydrogen intensity mapping'). The resulting maps of large-scale structure at redshifts 0.8-2.5 will be used to measure Baryon Acoustic Oscillations (BAO). HIRAX will improve upon current BAO measurements from galaxy surveys by observing a larger cosmological volume (larger in both survey area and redshift range) and by measuring BAO at higher redshift when the expansion of the universe transitioned to Dark Energy domination. HIRAX will complement CHIME, a hydrogen intensity mapping experiment in the Northern Hemisphere, by completing the sky coverage in the same redshift range. HIRAX's location in the Southern Hemisphere also allows a variety of cross-correlation measurements with large-scale structure surveys at many wavelengths. Daily maps of a few thousand square degrees of the Southern Hemisphere, encompassing much of the Milky Way galaxy, will also open new opportunities for discovering and monitoring radio transients. The HIRAX correlator will have the ability to rapidly and eXperimentciently detect transient events. This new data will shed light on the poorly understood nature of fast radio bursts (FRBs), enable pulsar monitoring to enhance long-wavelength gravitational wave searches, and provide a rich data set for new radio transient phenomena searches. This paper discusses the HIRAX instrument, science goals, and current status., Comment: 11 pages, 5 figures
Published: 2016
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9. The Q/U Imaging ExperimenT: Polarization Measurements of the Galactic Plane at 43 and 95 GHz

Author: QUIET Collaboration, Ruud, T. M., Fuskeland, U., Wehus, I. K., Vidal, M., Araujo, D., Bischoff, C., Buder, I., Chinone, Y., Cleary, K., Dumoulin, R. N., Kusaka, A., Monsalve, R., Naess, S. K., Newburgh, L. B., Reeves, R. A., Zwart, J. T. L., Bronfman, L., Davies, R. D., Davis, R., Dickinson, C., Eriksen, H. K., Gaier, T., Gundersen, J. O., Hasegawa, M., Hazumi, M., Huffenberger, K. M., Jones, M. E., Lawrence, C. R., Leitch, E. M., Limon, M., Miller, A. D., Pearson, T. J., Piccirillo, L., Radford, S. J. E., Readhead, A. C. S., Samtleben, D., Seiffert, M., Shepherd, M. C., Staggs, S. T., Tajima, O., and Thompson, K. L.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present polarization observations of two Galactic plane fields centered on Galactic coordinates (l,b)=(0 deg,0 deg) and (329 deg, 0 deg) at Q- (43 GHz) and W-band (95 GHz), covering between 301 and 539 square degrees depending on frequency and field. These measurements were made with the QUIET instrument between 2008 October and 2010 December, and include a total of 1263 hours of observations. The resulting maps represent the deepest large-area Galactic polarization observations published to date at the relevant frequencies with instrumental rms noise varying between 1.8 and 2.8 uK deg, 2.3-6 times deeper than corresponding WMAP and Planck maps. The angular resolution is 27.3' and 12.8' FWHM at Q- and W-band, respectively. We find excellent agreement between the QUIET and WMAP maps over the entire fields, and no compelling evidence for significant residual instrumental systematic errors in either experiment, whereas the Planck 44 GHz map deviates from these in a manner consistent with reported systematic uncertainties for this channel. We combine QUIET and WMAP data to compute inverse-variance-weighted average maps, effectively retaining small angular scales from QUIET and large angular scales from WMAP. From these combined maps, we derive constraints on several important astrophysical quantities, including a robust detection of polarized synchrotron spectral index steepening of ~0.2 off the plane, as well as the Faraday rotation measure toward the Galactic center (RM=-4000 +/- 200 rad m^-2), all of which are consistent with previously published results. Both the raw QUIET and the co-added QUIET+WMAP maps are made publicly available together with all necessary ancillary information., Comment: 22 pages, 18 figures; accepted for publication in ApJ; data are available on Lambda (http://lambda.gsfc.nasa.gov)
Published: 2015
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10. The Q/U Imaging Experiment: Polarization Measurements of Radio Sources at 43 and 95 GHz

Author: QUIET Collaboration, Huffenberger, K. M., Araujo, D., Bischoff, C., Buder, I., Chinone, Y., Cleary, K., Kusaka, A., Monsalve, R., Næss, S. K., Newburgh, L. B., Reeves, R., Ruud, T. M., Wehus, I. K., Zwart, J. T. L., Dickinson, C., Eriksen, H. K., Gaier, T., Gundersen, J. O., Hasegawa, M., Hazumi, M., Miller, A. D., Radford, S. J. E., Readhead, A. C. S., Staggs, S. T., Tajima, O., and Thompson, K. L.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present polarization measurements of extragalactic radio sources observed during the Cosmic Microwave Background polarization survey of the Q/U Imaging Experiment (QUIET), operating at 43 GHz (Q-band) and 95 GHz (W-band). We examine sources selected at 20 GHz from the public, $>$40 mJy catalog of the Australia Telescope (AT20G) survey. There are $\sim$480 such sources within QUIET's four low-foreground survey patches, including the nearby radio galaxies Centaurus A and Pictor A. The median error on our polarized flux density measurements is 30--40 mJy per Stokes parameter. At S/N $> 3$ significance, we detect linear polarization for seven sources in Q-band and six in W-band; only $1.3 \pm 1.1$ detections per frequency band are expected by chance. For sources without a detection of polarized emission, we find that half of the sources have polarization amplitudes below 90 mJy (Q-band) and 106 mJy (W-band), at 95% confidence. Finally, we compare our polarization measurements to intensity and polarization measurements of the same sources from the literature. For the four sources with WMAP and Planck intensity measurements $>1$ Jy, the polarization fraction are above 1% in both QUIET bands. At high significance, we compute polarization fractions as much as 10--20% for some sources, but the effects of source variability may cut that level in half for contemporaneous comparisons. Our results indicate that simple models---ones that scale a fixed polarization fraction with frequency---are inadequate to model the behavior of these sources and their contributions to polarization maps., Comment: 16 pages, 10 figures. Submitted to ApJ
Published: 2014
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11. The QUIET Instrument

Author: QUIET Collaboration, Bischoff, C., Brizius, A., Buder, I., Chinone, Y., Cleary, K., Dumoulin, R. N., Kusaka, A., Monsalve, R., Naess, S. K., Newburgh, L. B., Nixon, G., Reeves, R., Smith, K. M., Vanderlinde, K., Wehus, I. K., Bogdan, M., Bustos, R., Church, S. E., Davis, R., Dickinson, C., Eriksen, H. K., Gaier, T., Gundersen, J. O., Hasegawa, M., Hazumi, M., Holler, C., Huffenberger, K. M., Imbriale, W. A., Ishidoshiro, K., Jones, M. E., Kangaslahti, P., Kapner, D. J., Lawrence, C. R., Leitch, E. M., Limon, M., McMahon, J. J., Miller, A. D., Nagai, M., Nguyen, H., Pearson, T. J., Piccirillo, L., Radford, S. J. E., Readhead, A. C. S., Richards, J. L., Samtleben, D., Seiffert, M., Shepherd, M. C., Staggs, S. T., Tajima, O., Thompson, K. L., Williamson, R., Winstein, B., Wollack, E. J., and Zwart, J. T. L.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the Cosmic Microwave Background, targeting the imprint of inflationary gravitational waves at large angular scales (~ 1 degree). Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4 m side-fed Dragonian telescope. The polarimeters which form the focal planes use a highly compact design based on High Electron Mobility Transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 uK sqrt(s)) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r < 0.1. The 84-element W-band polarimeter array has a sensitivity of 87 uK sqrt(s) at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r < 0.01. The two arrays together cover multipoles in the range l= 25-975. These are the largest HEMT-based arrays deployed to date. This article describes the design, calibration, performance of, and sources of systematic error for the instrument.
Published: 2012
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12. Second Season QUIET Observations: Measurements of the CMB Polarization Power Spectrum at 95 GHz

Author: QUIET Collaboration, Araujo, D., Bischoff, C., Brizius, A., Buder, I., Chinone, Y., Cleary, K., Dumoulin, R. N., Kusaka, A., Monsalve, R., Næss, S. K., Newburgh, L. B., Reeves, R., Wehus, I. K., Zwart, J. T. L., Bronfman, L., Bustos, R., Church, S. E., Dickinson, C., Eriksen, H. K., Gaier, T., Gundersen, J. O., Hasegawa, M., Hazumi, M., Huffenberger, K. M., Ishidoshiro, K., Jones, M. E., Kangaslahti, P., Kapner, D. J., Kubik, D., Lawrence, C. R., Limon, M., McMahon, J. J., Miller, A. D., Nagai, M., Nguyen, H., Nixon, G., Pearson, T. J., Piccirillo, L., Radford, S. J. E., Readhead, A. C. S., Richards, J. L., Samtleben, D., Seiffert, M., Shepherd, M. C., Smith, K. M., Staggs, S. T., Tajima, O., Thompson, K. L., Vanderlinde, K., and Williamson, R.
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Q/U Imaging ExperimenT (QUIET) has observed the cosmic microwave background (CMB) at 43 and 95GHz. The 43-GHz results have been published in QUIET Collaboration et al. (2011), and here we report the measurement of CMB polarization power spectra using the 95-GHz data. This data set comprises 5337 hours of observations recorded by an array of 84 polarized coherent receivers with a total array sensitivity of 87 uK sqrt(s). Four low-foreground fields were observed, covering a total of ~1000 square degrees with an effective angular resolution of 12.8', allowing for constraints on primordial gravitational waves and high-signal-to-noise measurements of the E-modes across three acoustic peaks. The data reduction was performed using two independent analysis pipelines, one based on a pseudo-Cl (PCL) cross-correlation approach, and the other on a maximum-likelihood (ML) approach. All data selection criteria and filters were modified until a predefined set of null tests had been satisfied before inspecting any non-null power spectrum. The results derived by the two pipelines are in good agreement. We characterize the EE, EB and BB power spectra between l=25 and 975 and find that the EE spectrum is consistent with LCDM, while the BB power spectrum is consistent with zero. Based on these measurements, we constrain the tensor-to-scalar ratio to r=1.1+0.9-0.8 (r<2.8 at 95% C.L.) as derived by the ML pipeline, and r=1.2+0.9-0.8 (r<2.7 at 95% C.L.) as derived by the PCL pipeline. In one of the fields, we find a correlation with the dust component of the Planck Sky Model, though the corresponding excess power is small compared to statistical errors. Finally, we derive limits on all known systematic errors, and demonstrate that these correspond to a tensor-to-scalar ratio smaller than r=0.01, the lowest level yet reported in the literature., Comment: 10 pages, 6 figures, 3 tables, submitted to ApJ, This paper should be cited as "QUIET Collaboration (2012)." v2: updated to reflect published version
Published: 2012
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13. First Season QUIET Observations: Measurements of CMB Polarization Power Spectra at 43 GHz in the Multipole Range 25 <= ell <= 475

Author: QUIET Collaboration, Bischoff, C., Brizius, A., Buder, I., Chinone, Y., Cleary, K., Dumoulin, R. N., Kusaka, A., Monsalve, R., Næss, S. K., Newburgh, L. B., Reeves, R., Smith, K. M., Wehus, I. K., Zuntz, J. A., Zwart, J. T. L., Bronfman, L., Bustos, R., Church, S. E., Dickinson, C., Eriksen, H. K., Ferreira, P. G., Gaier, T., Gundersen, J. O., Hasegawa, M., Hazumi, M., Huffenberger, K. M., Jones, M. E., Kangaslahti, P., Kapner, D. J., Lawrence, C. R., Limon, M., May, J., McMahon, J. J., Miller, A. D., Nguyen, H., Nixon, G. W., Pearson, T. J., Piccirillo, L., Radford, S. J. E., Readhead, A. C. S., Richards, J. L., Samtleben, D., Seiffert, M., Shepherd, M. C., Staggs, S. T., Tajima, O., Thompson, K. L., Vanderlinde, K., Williamson, R., and Winstein, B.
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: The Q/U Imaging ExperimenT (QUIET) employs coherent receivers at 43GHz and 95GHz, operating on the Chajnantor plateau in the Atacama Desert in Chile, to measure the anisotropy in the polarization of the CMB. QUIET primarily targets the B modes from primordial gravitational waves. The combination of these frequencies gives sensitivity to foreground contributions from diffuse Galactic synchrotron radiation. Between 2008 October and 2010 December, >10,000hours of data were collected, first with the 19-element 43GHz array (3458hours) and then with the 90-element 95GHz array. Each array observes the same four fields, selected for low foregrounds, together covering ~1000deg^2. This paper reports initial results from the 43GHz receiver which has an array sensitivity to CMB fluctuations of 69uK sqrt(s). The data were extensively studied with a large suite of null tests before the power spectra, determined with two independent pipelines, were examined. Analysis choices, including data selection, were modified until the null tests passed. Cross correlating maps with different telescope pointings is used to eliminate a bias. This paper reports the EE, BB and EB power spectra in the multipole range ell=25-475. With the exception of the lowest multipole bin for one of the fields, where a polarized foreground, consistent with Galactic synchrotron radiation, is detected with 3sigma significance, the E-mode spectrum is consistent with the LCDM model, confirming the only previous detection of the first acoustic peak. The B-mode spectrum is consistent with zero, leading to a measurement of the tensor-to-scalar ratio of r=0.35+1.06-0.87. The combination of a new time-stream double-demodulation technique, Mizuguchi-Dragone optics, natural sky rotation, and frequent boresight rotation leads to the lowest level of systematic contamination in the B-mode power so far reported, below the level of r=0.1, Comment: 19 pages, 14 figures, higher quality figures are available at http://quiet.uchicago.edu/results/index.html; Fixed a typo and corrected statistical error values used as a reference in Figure 14, showing our systematic uncertainties (unchanged) vs. multipole; Revision to ApJ accepted version, this paper should be cited as "QUIET Collaboration et al. (2011)"
Published: 2010
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14. Erratum: Atacama Cosmology Telescope: Modeling the gas thermodynamics in BOSS CMASS galaxies from kinematic and thermal Sunyaev-Zel'dovich measurements (Phys. Rev. D (2021) 103 (063514) DOI: 10.1103/PhysRevD.103.063514)

Author: Amodeo S., Amodeo, S, Battaglia, N, Schaan, E, Ferraro, S, Moser, E, Aiola, S, Austermann, J, Beall, J, Bean, R, Becker, D, Bond, R, Calabrese, E, Calafut, V, Choi, S, Denison, E, Devlin, M, Duff, S, Duivenvoorden, A, Dunkley, J, Dünner, R, Gallardo, P, Hall, K, Han, D, Hill, J, Hilton, G, Hilton, M, Hložek, R, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Macinnis, A, Mcmahon, J, Madhavacheril, M, Moodley, K, Mroczkowski, T, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schillaci, A, Sehgal, N, Sifón, C, Spergel, D, Staggs, S, Storer, E, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Vavagiakis, E, Wollack, E, Xu, Z, Amodeo S., Battaglia N., Schaan E., Ferraro S., Moser E., Aiola S., Austermann J. E., Beall J. A., Bean R., Becker D. T., Bond R. J., Calabrese E., Calafut V., Choi S. K., Denison E. V., Devlin M., Duff S. M., Duivenvoorden A. J., Dunkley J., Dünner R., Gallardo P. A., Hall K. R., Han D., Hill J. C., Hilton G. C., Hilton M., HloŽek R., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Macinnis A., McMahon J., Madhavacheril M. S., Moodley K., Mroczkowski T., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schillaci A., Sehgal N., Sifón C., Spergel D. N., Staggs S., Storer E. R., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Vavagiakis E. M., Wollack E. J., Xu Z., Amodeo S., Amodeo, S, Battaglia, N, Schaan, E, Ferraro, S, Moser, E, Aiola, S, Austermann, J, Beall, J, Bean, R, Becker, D, Bond, R, Calabrese, E, Calafut, V, Choi, S, Denison, E, Devlin, M, Duff, S, Duivenvoorden, A, Dunkley, J, Dünner, R, Gallardo, P, Hall, K, Han, D, Hill, J, Hilton, G, Hilton, M, Hložek, R, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Macinnis, A, Mcmahon, J, Madhavacheril, M, Moodley, K, Mroczkowski, T, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schillaci, A, Sehgal, N, Sifón, C, Spergel, D, Staggs, S, Storer, E, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Vavagiakis, E, Wollack, E, Xu, Z, Amodeo S., Battaglia N., Schaan E., Ferraro S., Moser E., Aiola S., Austermann J. E., Beall J. A., Bean R., Becker D. T., Bond R. J., Calabrese E., Calafut V., Choi S. K., Denison E. V., Devlin M., Duff S. M., Duivenvoorden A. J., Dunkley J., Dünner R., Gallardo P. A., Hall K. R., Han D., Hill J. C., Hilton G. C., Hilton M., HloŽek R., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Macinnis A., McMahon J., Madhavacheril M. S., Moodley K., Mroczkowski T., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schillaci A., Sehgal N., Sifón C., Spergel D. N., Staggs S., Storer E. R., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Vavagiakis E. M., Wollack E. J., and Xu Z.
Published: 2023

15. Characterization and Performance of a Kilo-TES Sub-Array for ACTPol

Author: Grace, E. A., Beall, J., Cho, H. M., Devlin, M. J., Fox, A., Hilton, G., Hubmayr, J., Irwin, K., Klein, J., Li, D., Lungu, M., Newburgh, L. B., Nibarger, J., Niemack, M. D., McMahon, J., Page, L. A., Pappas, C., Schmitt, B. L., Staggs, S. T., Van Lanen, J., and Wollack, E.
Published: 2014
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16. Optical Efficiency and R(T,I) Measurements of ACTPol TESes Using Time Domain Multiplexing Electronics

Author: Pappas, C. G., Beall, J., Brevick, J., Cho, H. M., Devlin, M. J., Fox, A., Grace, E. A., Hilton, G. C., Hubmayr, J., Irwin, K. D., Klein, J., Li, D., Lungu, M., Newburgh, L. B., Nibarger, J. P., Niemack, M. D., McMahon, J. J., Page, L. A., Schmitt, B. L., Staggs, S. T., Van Lanen, J., and Wollack, E. J.
Published: 2014
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17. Foreground and RFI Mitigation with the Baryon Mapping experiment (BMX)

Author: Saliwanchik, B. R. B., primary, O'Connor, P., additional, Slosar, A., additional, Stankus, P., additional, Harris, M., additional, Haupt, J., additional, Kuczewski, J., additional, Kuhn, E. R., additional, Newburgh, L. B., additional, Polish, A., additional, Sheehy, C. D., additional, Troiani, G., additional, and Tyndall, W., additional
Published: 2021
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18. The Atacama Cosmology Telescope: Detection of the pairwise kinematic Sunyaev-Zel’dovich effect with SDSS DR15 galaxies

Author: Calafut, V., primary, Gallardo, P. A., additional, Vavagiakis, E. M., additional, Amodeo, S., additional, Aiola, S., additional, Austermann, J. E., additional, Battaglia, N., additional, Battistelli, E. S., additional, Beall, J. A., additional, Bean, R., additional, Bond, J. R., additional, Calabrese, E., additional, Choi, S. K., additional, Cothard, N. F., additional, Devlin, M. J., additional, Duell, C. J., additional, Duff, S. M., additional, Duivenvoorden, A. J., additional, Dunkley, J., additional, Dunner, R., additional, Ferraro, S., additional, Guan, Y., additional, Hill, J. C., additional, Hilton, G. C., additional, Hilton, M., additional, Hložek, R., additional, Huber, Z. B., additional, Hubmayr, J., additional, Huffenberger, K. M., additional, Hughes, J. P., additional, Koopman, B. J., additional, Kosowsky, A., additional, Li, Y., additional, Lokken, M., additional, Madhavacheril, M., additional, McMahon, J., additional, Moodley, K., additional, Naess, S., additional, Nati, F., additional, Newburgh, L. B., additional, Niemack, M. D., additional, Page, L. A., additional, Partridge, B., additional, Schaan, E., additional, Schillaci, A., additional, Sifón, C., additional, Spergel, D. N., additional, Staggs, S. T., additional, Ullom, J. N., additional, Vale, L. R., additional, Van Engelen, A., additional, Van Lanen, J., additional, Wollack, E. J., additional, and Xu, Z., additional
Published: 2021
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19. The Atacama Cosmology Telescope: Probing the baryon content of SDSS DR15 galaxies with the thermal and kinematic Sunyaev-Zel’dovich effects

Author: Vavagiakis, E. M., primary, Gallardo, P. A., additional, Calafut, V., additional, Amodeo, S., additional, Aiola, S., additional, Austermann, J. E., additional, Battaglia, N., additional, Battistelli, E. S., additional, Beall, J. A., additional, Bean, R., additional, Bond, J. R., additional, Calabrese, E., additional, Choi, S. K., additional, Cothard, N. F., additional, Devlin, M. J., additional, Duell, C. J., additional, Duff, S. M., additional, Duivenvoorden, A. J., additional, Dunkley, J., additional, Dunner, R., additional, Ferraro, S., additional, Guan, Y., additional, Hill, J. C., additional, Hilton, G. C., additional, Hilton, M., additional, Hložek, R., additional, Huber, Z. B., additional, Hubmayr, J., additional, Huffenberger, K. M., additional, Hughes, J. P., additional, Koopman, B. J., additional, Kosowsky, A., additional, Li, Y., additional, Lokken, M., additional, Madhavacheril, M., additional, McMahon, J., additional, Moodley, K., additional, Naess, S., additional, Nati, F., additional, Newburgh, L. B., additional, Niemack, M. D., additional, Page, L. A., additional, Partridge, B., additional, Schaan, E., additional, Schillaci, A., additional, Sifón, C., additional, Spergel, D. N., additional, Staggs, S. T., additional, Ullom, J. N., additional, Vale, L. R., additional, Van Engelen, A., additional, Van Lanen, J., additional, Wollack, E. J., additional, and Xu, Z., additional
Published: 2021
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20. An All Silicon Feedhorn-Coupled Focal Plane for Cosmic Microwave Background Polarimetry

Author: Hubmayr, J., Appel, J. W., Austermann, J. E., Beall, J. A., Becker, D., Benson, B. A., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Cho, H. M., Crites, A. T., Essinger-Hileman, T., Fox, A., George, E. M., Halverson, N. W., Harrington, N. L., Henning, J. W., Hilton, G. C., Holzapfel, W. L., Irwin, K. D., Lee, A. T., Li, D., McMahon, J., Mehl, J., Natoli, T., Niemack, M. D., Newburgh, L. B., Nibarger, J. P., Parker, L. P., Schmitt, B. L., Staggs, S. T., Van Lanen, J., Wollack, E. J., and Yoon, K. W.
Published: 2012
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21. Periodic activity from a fast radio burst source

Author: Amiri, M., Andersen, B. C., Bandura, K. M., Bhardwaj, M., Boyle, P. J., Brar, C., Chawla, P., Chen, T., Cliche, J. F., Cubranic, D., Deng, M., Denman, N. T., Dobbs, M., Dong, F. Q., Hill, A. S., Höfer, C., Josephy, A., Kania, J. W., Karuppusamy, R., Kaspi, V. M., Keimpema, A., Kirsten, F., Landecker, T. L., Lang, D. A., Leung, C., Li, D. Z., Lin, H.-H., Marcote, B., Masui, K. W., Mckinven, R., Mena-Parra, J., Merryfield, M., Michilli, D., Milutinovic, N., Mirhosseini, A., Naidu, A., Newburgh, L. B., Ng, C., Nimmo, K., Paragi, Z., Patel, C., Pen, U.-L., Pinsonneault-Marotte, T., Pleunis, Z., Rafiei-Ravandi, M, Rahman, M., Ransom, S. M., Renard, A., Sanghavi, P., Scholz, P., Shaw, J. R., Shin, K., Siegel, S. R., Singh, S., Smegal, R. J., Smith, K. M., Stairs, I. H., Tendulkar, S. P., Tretyakov, I., Vanderlinde, K., Wang, H., Wang, X., Wulf, D., Yadav, P., Zwaniga, A. V., The CHIME/FRB Collaboration, High Energy Astrophys. & Astropart. Phys (API, FNWI), Massachusetts Institute of Technology. Department of Mechanical Engineering, Massachusetts Institute of Technology. Department of Physics, and MIT Kavli Institute for Astrophysics and Space Research
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Multidisciplinary, 010308 nuclear & particles physics, Fast radio burst, Canadian Hydrogen Intensity Mapping Experiment, Phase (waves), FOS: Physical sciences, Cosmic ray, Astrophysics, 01 natural sciences, Modulation, 0103 physical sciences, Regular pattern, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: Fast radio bursts (FRBs) are bright, millisecond-duration radio transients originating from sources at extragalactic distances1, the origin of which is unknown. Some FRB sources emit repeat bursts, ruling out cataclysmic origins for those events2,3,4. Despite searches for periodicity in repeat burst arrival times on timescales from milliseconds to many days2,5,6,7, these bursts have hitherto been observed to appear sporadically and—although clustered8—without a regular pattern. Here we report observations of a 16.35 ± 0.15 day periodicity (or possibly a higher-frequency alias of that periodicity) from the repeating FRB 180916.J0158+65 detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project4,9. In 38 bursts recorded from 16 September 2018 to 4 February 2020 UTC, we find that all bursts arrive in a five-day phase window, and 50 per cent of the bursts arrive in a 0.6-day phase window. Our results suggest a mechanism for periodic modulation either of the burst emission itself or through external amplification or absorption, and disfavour models invoking purely sporadic processes.
Published: 2020

22. The atacama cosmology telescope: A catalog of >4000 Sunyaev–Zel’dovich galaxy clusters

Author: Hilton, M, Sifon, C, Naess, S, Madhavacheril, M, Oguri, M, Rozo, E, Rykoff, E, Adhikari, S, Aguena, M, Aiola, S, Allam, S, Amodeo, S, Amon, A, Annis, J, Ansarinejad, B, Abbott, T, Aros-Bunster, C, Austermann, J, Avila, S, Bacon, D, Battaglia, N, Beall, J, Becker, D, Bernstein, G, Bertin, E, Bhandarkar, T, Bhargava, S, Bond, J, Brooks, D, Burke, D, Calabrese, E, Carrasco Kind, M, Carretero, J, Choi, S, Choi, A, Conselice, C, Da Costa, L, Costanzi, M, Crichton, D, Crowley, K, Dunner, R, Denison, E, Devlin, M, Dicker, S, Diehl, H, Dietrich, J, Doel, P, Duff, S, Duivenvoorden, A, Dunkley, J, Everett, S, Ferraro, S, Ferte, A, Flaugher, B, Frieman, J, Ferrero, I, Gallardo, P, Garcia-Bellido, J, Gaztanaga, E, Giles, P, Golec, J, Gralla, M, Grandis, S, Gruen, D, Gerdes, D, Gruendl, R, Gschwend, J, Gutierrez, G, Han, D, Hartley, W, Hasselfield, M, Hill, J, Hilton, G, Hincks, A, Hinton, S, Ho, S, Honscheid, K, Hoyle, B, Hubmayr, J, Huffenberger, K, Hughes, J, Jaelani, A, Jain, B, James, D, Jeltema, T, Kent, S, Knowles, K, Koopman, B, Kuehn, K, Lahav, O, Lima, M, Lin, Y, Lokken, M, Loubser, S, Maccrann, N, Maia, M, Marriage, T, Martin, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Moodley, K, Morgan, R, Mroczkowski, T, Nati, F, Newburgh, L, Niemack, M, Nishizawa, A, Miyatake, H, Ogando, R, Orlowski-Scherer, J, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Phakathi, P, Plazas, A, Robertson, N, Romer, A, Carnero Rosell, A, Sanchez, E, Schaan, E, Schillaci, A, Sehgal, N, Serrano, S, Shin, T, Simon, S, Smith, M, Salatino, M, Soares-Santos, M, Spergel, D, Staggs, S, Storer, E, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Trac, H, Ullom, J, Vale, L, Van Lanen, J, Vavagiakis, E, De Vicente, J, Wilkinson, R, Wollack, E, Xu, Z, Zhan, Y, Hilton M., Sifon C., Naess S., Madhavacheril M., Oguri M., Rozo E., Rykoff E., Adhikari S., Aguena M., Aiola S., Allam S., Amodeo S., Amon A., Annis J., Ansarinejad B., Abbott T. M. C., Aros-Bunster C., Austermann J. E., Avila S., Bacon D., Battaglia N., Beall J. A., Becker D. T., Bernstein G. M., Bertin E., Bhandarkar T., Bhargava S., Bond J. R., Brooks D., Burke D. L., Calabrese E., Carrasco Kind M., Carretero J., Choi S. K., Choi A., Conselice C., Da Costa L. N., Costanzi M., Crichton D., Crowley K. T., Dunner R., Denison E. V., Devlin M. J., Dicker S. R., Diehl H. T., Dietrich J. P., Doel P., Duff S. M., Duivenvoorden A. J., Dunkley J., Everett S., Ferraro S., Ferte A., Flaugher B., Frieman J., Ferrero I., Gallardo P. A., Garcia-Bellido J., Gaztanaga E., Giles P., Golec J. E., Gralla M. B., Grandis S., Gruen D., Gerdes D. W., Gruendl R. A., Gschwend J., Gutierrez G., Han D., Hartley W. G., Hasselfield M., Hill J. C., Hilton G. C., Hincks A. D., Hinton S. R., Ho S. -P. P., Honscheid K., Hoyle B., Hubmayr J., Huffenberger K. M., Hughes J. P., Jaelani A. T., Jain B., James D. J., Jeltema T., Kent S., Knowles K., Koopman B. J., Kuehn K., Lahav O., Lima M., Lin Y. -T., Lokken M., Loubser S. I., MacCrann N., Maia M. A. G., Marriage T. A., Martin J., McMahon J., Melchior P., Menanteau F., Miquel R., Moodley K., Morgan R., Mroczkowski T., Nati F., Newburgh L. B., Niemack M. D., Nishizawa A. J., Miyatake H., Ogando R. L. C., Orlowski-Scherer J., Page L. A., Palmese A., Partridge B., Paz-Chinchon F., Phakathi P., Plazas A. A., Robertson N. C., Romer A. K., Carnero Rosell A., Sanchez E., Schaan E., Schillaci A., Sehgal N., Serrano S., Shin T., Simon S. M., Smith M., Salatino M., Soares-Santos M., Spergel D. N., Staggs S. T., Storer E. R., Suchyta E., Swanson M. E. C., Tarle G., Thomas D., To C., Trac H., Ullom J. N., Vale L. R., Van Lanen J., Vavagiakis E. M., De Vicente J., Wilkinson R. D., Wollack E. J., Xu Z., Zhan Y., Hilton, M, Sifon, C, Naess, S, Madhavacheril, M, Oguri, M, Rozo, E, Rykoff, E, Adhikari, S, Aguena, M, Aiola, S, Allam, S, Amodeo, S, Amon, A, Annis, J, Ansarinejad, B, Abbott, T, Aros-Bunster, C, Austermann, J, Avila, S, Bacon, D, Battaglia, N, Beall, J, Becker, D, Bernstein, G, Bertin, E, Bhandarkar, T, Bhargava, S, Bond, J, Brooks, D, Burke, D, Calabrese, E, Carrasco Kind, M, Carretero, J, Choi, S, Choi, A, Conselice, C, Da Costa, L, Costanzi, M, Crichton, D, Crowley, K, Dunner, R, Denison, E, Devlin, M, Dicker, S, Diehl, H, Dietrich, J, Doel, P, Duff, S, Duivenvoorden, A, Dunkley, J, Everett, S, Ferraro, S, Ferte, A, Flaugher, B, Frieman, J, Ferrero, I, Gallardo, P, Garcia-Bellido, J, Gaztanaga, E, Giles, P, Golec, J, Gralla, M, Grandis, S, Gruen, D, Gerdes, D, Gruendl, R, Gschwend, J, Gutierrez, G, Han, D, Hartley, W, Hasselfield, M, Hill, J, Hilton, G, Hincks, A, Hinton, S, Ho, S, Honscheid, K, Hoyle, B, Hubmayr, J, Huffenberger, K, Hughes, J, Jaelani, A, Jain, B, James, D, Jeltema, T, Kent, S, Knowles, K, Koopman, B, Kuehn, K, Lahav, O, Lima, M, Lin, Y, Lokken, M, Loubser, S, Maccrann, N, Maia, M, Marriage, T, Martin, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Moodley, K, Morgan, R, Mroczkowski, T, Nati, F, Newburgh, L, Niemack, M, Nishizawa, A, Miyatake, H, Ogando, R, Orlowski-Scherer, J, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Phakathi, P, Plazas, A, Robertson, N, Romer, A, Carnero Rosell, A, Sanchez, E, Schaan, E, Schillaci, A, Sehgal, N, Serrano, S, Shin, T, Simon, S, Smith, M, Salatino, M, Soares-Santos, M, Spergel, D, Staggs, S, Storer, E, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Trac, H, Ullom, J, Vale, L, Van Lanen, J, Vavagiakis, E, De Vicente, J, Wilkinson, R, Wollack, E, Xu, Z, Zhan, Y, Hilton M., Sifon C., Naess S., Madhavacheril M., Oguri M., Rozo E., Rykoff E., Adhikari S., Aguena M., Aiola S., Allam S., Amodeo S., Amon A., Annis J., Ansarinejad B., Abbott T. M. C., Aros-Bunster C., Austermann J. E., Avila S., Bacon D., Battaglia N., Beall J. A., Becker D. T., Bernstein G. M., Bertin E., Bhandarkar T., Bhargava S., Bond J. R., Brooks D., Burke D. L., Calabrese E., Carrasco Kind M., Carretero J., Choi S. K., Choi A., Conselice C., Da Costa L. N., Costanzi M., Crichton D., Crowley K. T., Dunner R., Denison E. V., Devlin M. J., Dicker S. R., Diehl H. T., Dietrich J. P., Doel P., Duff S. M., Duivenvoorden A. J., Dunkley J., Everett S., Ferraro S., Ferte A., Flaugher B., Frieman J., Ferrero I., Gallardo P. A., Garcia-Bellido J., Gaztanaga E., Giles P., Golec J. E., Gralla M. B., Grandis S., Gruen D., Gerdes D. W., Gruendl R. A., Gschwend J., Gutierrez G., Han D., Hartley W. G., Hasselfield M., Hill J. C., Hilton G. C., Hincks A. D., Hinton S. R., Ho S. -P. P., Honscheid K., Hoyle B., Hubmayr J., Huffenberger K. M., Hughes J. P., Jaelani A. T., Jain B., James D. J., Jeltema T., Kent S., Knowles K., Koopman B. J., Kuehn K., Lahav O., Lima M., Lin Y. -T., Lokken M., Loubser S. I., MacCrann N., Maia M. A. G., Marriage T. A., Martin J., McMahon J., Melchior P., Menanteau F., Miquel R., Moodley K., Morgan R., Mroczkowski T., Nati F., Newburgh L. B., Niemack M. D., Nishizawa A. J., Miyatake H., Ogando R. L. C., Orlowski-Scherer J., Page L. A., Palmese A., Partridge B., Paz-Chinchon F., Phakathi P., Plazas A. A., Robertson N. C., Romer A. K., Carnero Rosell A., Sanchez E., Schaan E., Schillaci A., Sehgal N., Serrano S., Shin T., Simon S. M., Smith M., Salatino M., Soares-Santos M., Spergel D. N., Staggs S. T., Storer E. R., Suchyta E., Swanson M. E. C., Tarle G., Thomas D., To C., Trac H., Ullom J. N., Vale L. R., Van Lanen J., Vavagiakis E. M., De Vicente J., Wilkinson R. D., Wollack E. J., Xu Z., and Zhan Y.
Abstract: We present a catalog of 4195 optically confirmed Sunyaev–Zel’dovich (SZ) selected galaxy clusters detected with signal-to-noise ratio >4 in 13,211 deg2 of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multifrequency matched filter to 98 and 150 GHz maps constructed from ACT observations obtained from 2008 to 2018 and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04 < z < 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ signal versus mass-scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M500c > 3.8 × 1014 Me, evaluated at z = 0.5, for clusters detected at signal-to-noise ratio >5 in maps filtered at an angular scale of 2 4. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ signal mass-scaling relation, such as the Dark Energy Survey (4566 deg2), the Hyper Suprime-Cam Subaru Strategic Program (469 deg2), and the Kilo Degree Survey (825 deg2). We highlight some noteworthy objects in the sample, including potentially projected systems, clusters with strong lensing features, clusters with active central galaxies or star formation, and systems of multiple clusters that may be physically associated. The cluster catalog will be a useful resource for future cosmological analyses and studying the evolution of the intracluster medium and galaxies in massive clusters over the past 10 Gyr.
Published: 2021

23. Erratum: The Simons Observatory Large Aperture Telescope Receiver (ApJS (2021) 256: 23 DOI: 10.3847/1538-4365/ac0db7)

Author: Zhu N., Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dunner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keating, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Zhu N., Bhandarkar T., Coppi G., Kofman A. M., Orlowski-Scherer J. L., Xu Z., Adachi S., Ade P., Aiola S., Austermann J., Bazarko A. O., Beall J. A., Bhimani S., Bond J. R., Chesmore G. E., Choi S. K., Connors J., Cothard N. F., Devlin M., Dicker S., Dober B., Duell C. J., Duff S. M., Dunner R., Fabbian G., Galitzki N., Gallardo P. A., Golec J. E., Haridas S. K., Harrington K., Healy E., Patty Ho S. -P., Huber Z. B., Hubmayr J., Iuliano J., Johnson B. R., Keating B., Kiuchi K., Koopman B. J., Lashner J., Lee A. T., Li Y., Limon M., Link M., Lucas T. J., McCarrick H., Moore J., Nati F., Newburgh L. B., Niemack M. D., Pierpaoli E., Randall M. J., Sarmiento K. P., Saunders L. J., Seibert J., Sierra C., Sonka R., Spisak J., Sutariya S., Tajima O., Teply G. P., Thornton R. J., Tsan T., Tucker C., Ullom J., Vavagiakis E. M., Vissers M. R., Walker S., Westbrook B., Wollack E. J., Zannoni M., Zhu N., Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dunner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keating, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Zhu N., Bhandarkar T., Coppi G., Kofman A. M., Orlowski-Scherer J. L., Xu Z., Adachi S., Ade P., Aiola S., Austermann J., Bazarko A. O., Beall J. A., Bhimani S., Bond J. R., Chesmore G. E., Choi S. K., Connors J., Cothard N. F., Devlin M., Dicker S., Dober B., Duell C. J., Duff S. M., Dunner R., Fabbian G., Galitzki N., Gallardo P. A., Golec J. E., Haridas S. K., Harrington K., Healy E., Patty Ho S. -P., Huber Z. B., Hubmayr J., Iuliano J., Johnson B. R., Keating B., Kiuchi K., Koopman B. J., Lashner J., Lee A. T., Li Y., Limon M., Link M., Lucas T. J., McCarrick H., Moore J., Nati F., Newburgh L. B., Niemack M. D., Pierpaoli E., Randall M. J., Sarmiento K. P., Saunders L. J., Seibert J., Sierra C., Sonka R., Spisak J., Sutariya S., Tajima O., Teply G. P., Thornton R. J., Tsan T., Tucker C., Ullom J., Vavagiakis E. M., Vissers M. R., Walker S., Westbrook B., Wollack E. J., and Zannoni M.
Abstract: After the publication of the article, it was brought to our attention that the description of Equation (1) may cause potential confusion. Thus, we have decided to provide a newer reference and added a unit for qtot in the description. The updated paragraph should read as the following:.
Published: 2021

24. The atacama cosmology telescope: Summary of dr4 and dr5 data products and data access

Author: Mallaby-Kay, M, Atkins, Z, Aiola, S, Amodeo, S, Austermann, J, Beall, J, Becker, D, Bond, J, Calabrese, E, Chesmore, G, Choi, S, Crowley, K, Darwish, O, Denison, E, Devlin, M, Duff, S, Duivenvoorden, A, Dunkley, J, Ferraro, S, Fichman, K, Gallardo, P, Golec, J, Guan, Y, Han, D, Hasselfield, M, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Louis, T, Macinnis, A, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Nibarger, J, Niemack, M, Page, L, Salatino, M, Schaan, E, Schillaci, A, Sehgal, N, Sherwin, B, Sifon, C, Simon, S, Staggs, S, Storer, E, Ullom, J, Van Engelen, A, Van Lanen, J, Vale, L, Wollack, E, Xu, Z, Mallaby-Kay M., Atkins Z., Aiola S., Amodeo S., Austermann J. E., Beall J. A., Becker D. T., Bond J. R., Calabrese E., Chesmore G. E., Choi S. K., Crowley K. T., Darwish O., Denison E. V., Devlin M. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Ferraro S., Fichman K., Gallardo P. A., Golec J. E., Guan Y., Han D., Hasselfield M., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Louis T., MacInnis A., Madhavacheril M. S., McMahon J., Moodley K., Naess S., Namikawa T., Nati F., Newburgh L. B., Nibarger J. P., Niemack M. D., Page L. A., Salatino M., Schaan E., Schillaci A., Sehgal N., Sherwin B. D., Sifon C., Simon S., Staggs S. T., Storer E. R., Ullom J. N., Van Engelen A., Van Lanen J., Vale L. R., Wollack E. J., Xu Z., Mallaby-Kay, M, Atkins, Z, Aiola, S, Amodeo, S, Austermann, J, Beall, J, Becker, D, Bond, J, Calabrese, E, Chesmore, G, Choi, S, Crowley, K, Darwish, O, Denison, E, Devlin, M, Duff, S, Duivenvoorden, A, Dunkley, J, Ferraro, S, Fichman, K, Gallardo, P, Golec, J, Guan, Y, Han, D, Hasselfield, M, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Louis, T, Macinnis, A, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Nibarger, J, Niemack, M, Page, L, Salatino, M, Schaan, E, Schillaci, A, Sehgal, N, Sherwin, B, Sifon, C, Simon, S, Staggs, S, Storer, E, Ullom, J, Van Engelen, A, Van Lanen, J, Vale, L, Wollack, E, Xu, Z, Mallaby-Kay M., Atkins Z., Aiola S., Amodeo S., Austermann J. E., Beall J. A., Becker D. T., Bond J. R., Calabrese E., Chesmore G. E., Choi S. K., Crowley K. T., Darwish O., Denison E. V., Devlin M. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Ferraro S., Fichman K., Gallardo P. A., Golec J. E., Guan Y., Han D., Hasselfield M., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Louis T., MacInnis A., Madhavacheril M. S., McMahon J., Moodley K., Naess S., Namikawa T., Nati F., Newburgh L. B., Nibarger J. P., Niemack M. D., Page L. A., Salatino M., Schaan E., Schillaci A., Sehgal N., Sherwin B. D., Sifon C., Simon S., Staggs S. T., Storer E. R., Ullom J. N., Van Engelen A., Van Lanen J., Vale L. R., Wollack E. J., and Xu Z.
Abstract: Two recent large data releases for the Atacama Cosmology Telescope (ACT), called DR4 and DR5, are available for public access. These data include temperature and polarization maps that cover nearly half the sky at arcminute resolution in three frequency bands; lensing maps and component-separated maps covering ~2100 deg2 of sky; derived power spectra and cosmological likelihoods; a catalog of over 4000 galaxy clusters; and supporting ancillary products including beam functions and masks. The data and products are described in a suite of ACT papers; here we provide a summary. In order to facilitate ease of access to these data, we present a set of Jupyter IPython notebooks developed to introduce users to DR4, DR5, and the tools needed to analyze these data. The data products (excluding simulations) and the set of notebooks are publicly available on the NASA Legacy Archive for Microwave Background Data Analysis; simulation products are available on the National Energy Research Scientific Computing Center.
Published: 2021

25. The Atacama Cosmology Telescope: Probing the baryon content of SDSS DR15 galaxies with the thermal and kinematic Sunyaev-Zel’dovich effects

Author: Vavagiakis, E, Gallardo, P, Calafut, V, Amodeo, S, Aiola, S, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Bond, J, Calabrese, E, Choi, S, Cothard, N, Devlin, M, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Guan, Y, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, Li, Y, Lokken, M, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schaan, E, Schillaci, A, Sifon, C, Spergel, D, Staggs, S, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Wollack, E, Xu, Z, Vavagiakis E. M., Gallardo P. A., Calafut V., Amodeo S., Aiola S., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Bond J. R., Calabrese E., Choi S. K., Cothard N. F., Devlin M. J., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Guan Y., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., Li Y., Lokken M., Madhavacheril M., McMahon J., Moodley K., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schaan E., Schillaci A., Sifon C., Spergel D. N., Staggs S. T., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Wollack E. J., Xu Z., Vavagiakis, E, Gallardo, P, Calafut, V, Amodeo, S, Aiola, S, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Bond, J, Calabrese, E, Choi, S, Cothard, N, Devlin, M, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Guan, Y, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, Li, Y, Lokken, M, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schaan, E, Schillaci, A, Sifon, C, Spergel, D, Staggs, S, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Wollack, E, Xu, Z, Vavagiakis E. M., Gallardo P. A., Calafut V., Amodeo S., Aiola S., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Bond J. R., Calabrese E., Choi S. K., Cothard N. F., Devlin M. J., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Guan Y., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., Li Y., Lokken M., Madhavacheril M., McMahon J., Moodley K., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schaan E., Schillaci A., Sifon C., Spergel D. N., Staggs S. T., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Wollack E. J., and Xu Z.
Abstract: We present measurements of the average thermal Sunyaev Zel’dovich (tSZ) effect from optically selected galaxy groups and clusters at high signal-to-noise (up to ) and estimate their baryon content within a radius aperture. Sources from the Sloan Digital Sky Survey Baryon Oscillation Spectroscopic Survey DR15 catalog overlap with 3,700 sq deg of sky observed by the Atacama Cosmology Telescope (ACT) from 2008 to 2018 at 150 and 98 GHz (ACT DR5), and 2,089 sq deg of internal linear combination component-separated maps combining ACT and Planck data (ACT DR4). The corresponding optical depths , which depend on the baryon content of the halos, are estimated using results from cosmological hydrodynamic simulations assuming an active galactic nuclei feedback radiative cooling model. We estimate the mean mass of the halos in multiple luminosity bins, and compare the tSZ-based estimates to theoretical predictions of the baryon content for a Navarro-Frenk-White profile. We do the same for estimates extracted from fits to pairwise baryon momentum measurements of the kinematic Sunyaev-Zel’dovich effect (kSZ) for the same dataset obtained in a companion paper. We find that the estimates from the tSZ measurements in this work and the kSZ measurements in the companion paper agree within for two out of the three disjoint luminosity bins studied, while they differ by in the highest luminosity bin. The optical depth estimates account for one-third to all of the theoretically predicted baryon content in the halos across luminosity bins. Potential systematic uncertainties are discussed. The tSZ and kSZ measurements provide a step toward empirical Compton- relationships to provide new tests of cluster formation and evolution models.
Published: 2021

26. The Atacama Cosmology Telescope: Detection of the pairwise kinematic Sunyaev-Zel’dovich effect with SDSS DR15 galaxies ()

Author: Calafut, V, Gallardo, P, Vavagiakis, E, Amodeo, S, Aiola, S, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Bond, J, Calabrese, E, Choi, S, Cothard, N, Devlin, M, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Guan, Y, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, Li, Y, Lokken, M, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schaan, E, Schillaci, A, Sifon, C, Spergel, D, Staggs, S, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Wollack, E, Xu, Z, Calafut V., Gallardo P. A., Vavagiakis E. M., Amodeo S., Aiola S., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Bond J. R., Calabrese E., Choi S. K., Cothard N. F., Devlin M. J., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Guan Y., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., Li Y., Lokken M., Madhavacheril M., McMahon J., Moodley K., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schaan E., Schillaci A., Sifon C., Spergel D. N., Staggs S. T., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Wollack E. J., Xu Z., Calafut, V, Gallardo, P, Vavagiakis, E, Amodeo, S, Aiola, S, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Bond, J, Calabrese, E, Choi, S, Cothard, N, Devlin, M, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Guan, Y, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, Li, Y, Lokken, M, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schaan, E, Schillaci, A, Sifon, C, Spergel, D, Staggs, S, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Wollack, E, Xu, Z, Calafut V., Gallardo P. A., Vavagiakis E. M., Amodeo S., Aiola S., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Bond J. R., Calabrese E., Choi S. K., Cothard N. F., Devlin M. J., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Guan Y., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., Li Y., Lokken M., Madhavacheril M., McMahon J., Moodley K., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schaan E., Schillaci A., Sifon C., Spergel D. N., Staggs S. T., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Wollack E. J., and Xu Z.
Abstract: We present a detection of the pairwise kinematic Sunyaev-Zeldovich (kSZ) effect using Atacama Cosmology Telescope (ACT) and Planck CMB observations in combination with Luminous Red Galaxy samples from the Sloan Digital Sky Survey (SDSS) DR15 catalog. Results are obtained using three ACT CMB maps: co-added 150 and 98 GHz maps, combining observations from 2008-2018 (ACT DR5), which overlap with SDSS DR15 over 3,700 sq. deg., and a component-separated map using night-time only observations from 2014-2015 (ACT DR4), overlapping with SDSS DR15 over 2,089 sq. deg. Comparisons of the results from these three maps provide consistency checks in relation to potential frequency-dependent foreground contamination. A total of 343,647 galaxies are used as tracers to identify and locate galaxy groups and clusters from which the kSZ signal is extracted using aperture photometry. We consider the impact of various aperture photometry assumptions and covariance estimation methods on the signal extraction. Theoretical predictions of the pairwise velocities are used to obtain best-fit, mass-averaged, optical depth estimates for each of five luminosity-selected tracer samples. A comparison of the kSZ-derived optical depth measurements obtained here to those derived from the thermal SZ effect for the same sample is presented in a companion paper.
Published: 2021

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

Author: 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., To C. -H., Wollack E., Wu H. -Y., 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., Vale L. R., 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., To C. -H., Wollack E., Wu H. -Y., 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.
Abstract: 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.
Published: 2021

28. MERGHERS pilot: MeerKAT discovery of diffuse emission in nine massive Sunyaev–Zel’dovich-selected galaxy clusters from ACT

Author: Knowles, K, primary, Pillay, D S, additional, Amodeo, S, additional, Baker, A J, additional, Basu, K, additional, Crichton, D, additional, de Gasperin, F, additional, Devlin, M, additional, Ferrari, C, additional, Hilton, M, additional, Huffenberger, K M, additional, Hughes, J P, additional, Koopman, B J, additional, Moodley, K, additional, Mroczkowski, T, additional, Naess, S, additional, Nati, F, additional, Newburgh, L B, additional, Oozeer, N, additional, Page, L, additional, Partridge, B, additional, Pfrommer, C, additional, Salatino, M, additional, Schillaci, A, additional, Sifón, C, additional, Smirnov, O, additional, Sikhosana, S P, additional, Wollack, E J, additional, and Xu, Z, additional
Published: 2021
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29. The Atacama Cosmology Telescope: A Catalog of >4000 Sunyaev–Zel’dovich Galaxy Clusters

Author: Hilton, M., primary, Sifón, C., additional, Naess, S., additional, Madhavacheril, M., additional, Oguri, M., additional, Rozo, E., additional, Rykoff, E., additional, Abbott, T. M. C., additional, Adhikari, S., additional, Aguena, M., additional, Aiola, S., additional, Allam, S., additional, Amodeo, S., additional, Amon, A., additional, Annis, J., additional, Ansarinejad, B., additional, Aros-Bunster, C., additional, Austermann, J. E., additional, Avila, S., additional, Bacon, D., additional, Battaglia, N., additional, Beall, J. A., additional, Becker, D. T., additional, Bernstein, G. M., additional, Bertin, E., additional, Bhandarkar, T., additional, Bhargava, S., additional, Bond, J. R., additional, Brooks, D., additional, Burke, D. L., additional, Calabrese, E., additional, Carrasco Kind, M., additional, Carretero, J., additional, Choi, S. K., additional, Choi, A., additional, Conselice, C., additional, Costa, L. N. da, additional, Costanzi, M., additional, Crichton, D., additional, Crowley, K. T., additional, Dünner, R., additional, Denison, E. V., additional, Devlin, M. J., additional, Dicker, S. R., additional, Diehl, H. T., additional, Dietrich, J. P., additional, Doel, P., additional, Duff, S. M., additional, Duivenvoorden, A. J., additional, Dunkley, J., additional, Everett, S., additional, Ferraro, S., additional, Ferrero, I., additional, Ferté, A., additional, Flaugher, B., additional, Frieman, J., additional, Gallardo, P. A., additional, García-Bellido, J., additional, Gaztanaga, E., additional, Gerdes, D. W., additional, Giles, P., additional, Golec, J. E., additional, Gralla, M. B., additional, Grandis, S., additional, Gruen, D., additional, Gruendl, R. A., additional, Gschwend, J., additional, Gutierrez, G., additional, Han, D., additional, Hartley, W. G., additional, Hasselfield, M., additional, Hill, J. C., additional, Hilton, G. C., additional, Hincks, A. D., additional, Hinton, S. R., additional, Ho, S-P. P., additional, Honscheid, K., additional, Hoyle, B., additional, Hubmayr, J., additional, Huffenberger, K. M., additional, Hughes, J. P., additional, Jaelani, A. T., additional, Jain, B., additional, James, D. J., additional, Jeltema, T., additional, Kent, S., additional, Knowles, K., additional, Koopman, B. J., additional, Kuehn, K., additional, Lahav, O., additional, Lima, M., additional, Lin, Y-T., additional, Lokken, M., additional, Loubser, S. I., additional, MacCrann, N., additional, Maia, M. A. G., additional, Marriage, T. A., additional, Martin, J., additional, McMahon, J., additional, Melchior, P., additional, Menanteau, F., additional, Miquel, R., additional, Miyatake, H., additional, Moodley, K., additional, Morgan, R., additional, Mroczkowski, T., additional, Nati, F., additional, Newburgh, L. B., additional, Niemack, M. D., additional, Nishizawa, A. J., additional, Ogando, R. L. C., additional, Orlowski-Scherer, J., additional, Page, L. A., additional, Palmese, A., additional, Partridge, B., additional, Paz-Chinchón, F., additional, Phakathi, P., additional, Plazas, A. A., additional, Robertson, N. C., additional, Romer, A. K., additional, Rosell, A. Carnero, additional, Salatino, M., additional, Sanchez, E., additional, Schaan, E., additional, Schillaci, A., additional, Sehgal, N., additional, Serrano, S., additional, Shin, T., additional, Simon, S. M., additional, Smith, M., additional, Soares-Santos, M., additional, Spergel, D. N., additional, Staggs, S. T., additional, Storer, E. R., additional, Suchyta, E., additional, Swanson, M. E. C., additional, Tarle, G., additional, Thomas, D., additional, To, C., additional, Trac, H., additional, Ullom, J. N., additional, Vale, L. R., additional, Lanen, J. Van, additional, Vavagiakis, E. M., additional, Vicente, J. De, additional, Wilkinson, R. D., additional, Wollack, E. J., additional, Xu, Z., additional, and Zhang, Y., additional
Published: 2021
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30. An All Silicon Feedhorn-Coupled Focal Plane for Cosmic Microwave Background Polarimetry

Author: Hubmayr, J, Appel, J. W, Austermann, J. E, Beall, J. A, Becker, D, Benson, B. A, Bleem, L. E, Carlstrom, J. E, Chang, C. L, Cho, H. M, Crites, A. T, Essinger-Hileman, T, Fox, A, George, E. M, Halverson, N. W, Harrington, N. L, Henning, J. W, Hilton, G. C, Irwin, K. D, Li, D, Niemack, M. D, Nibarger, J. P, VanLanen, J, Newburgh, L. B, and Parker, L. P
Subjects: Astronomy
Abstract: Upcoming experiments aim to produce high fidelity polarization maps of the cosmic microwave background. To achieve the required sensitivity, we are developing monolithic, feedhorn-coupled transition edge sensor polarimeter arrays operating at 150 GHz. We describe this focal plane architecture and the current status of this technology, focusing on single-pixel polarimeters being deployed on the Atacama B-mode Search (ABS) and an 84-pixel demonstration feedhorn array backed by four 10-pixel polarimeter arrays. The feedhorn array exhibits symmetric beams, cross-polar response less than -23 dB and excellent uniformity across the array. Monolithic polarimeter arrays, including arrays of silicon feedhorns, will be used in the Atacama Cosmology Telescope Polarimeter (ACTPol) and the South Pole Telescope Polarimeter (SPTpol) and have been proposed for upcoming balloon-borne instruments.
Published: 2011
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31. Periodic activity from a fast radio burst source

Author: Massachusetts Institute of Technology. Department of Mechanical Engineering, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, CHIME/FRB Collaboration, Amiri, M., Andersen, B. C., Bandura, K. M., Bhardwaj, M., Boyle, P. J., Brar, C., Chawla, P., Chen, Ting, Cliche, J. F., Cubranic, D., Deng, M., Denman, N. T., Dobbs, M., Dong, F. Q., Fandino, M., Fonseca, E., Gaensler, B. M., Giri, U., Good, D. C., Halpern, M., Hessels, J. W. T., Hill, A. S., Hofer, C., Josephy, A., Kania, J. W., Karuppusamy, R., Kaspi, V. M., Keimpema, A., Kirsten, F., Landecker, T. L., Lang, D. A., Leung, Calvin, Li, D. Z., Lin, H.-H., Marcote, B., Masui, Kiyoshi, Mckinven, R., Mena Parra, Juan David, Merryfield, M., Michilli, D., Milutinovic, N., Mirhosseini, A., Naidu, A., Newburgh, L. B., Ng, C., Nimmo, K., Paragi, Z., Patel, C., Pen, U.-L., Pinsonneault-Marotte, T., Pleunis, Z., Rafiei- Ravandi, M., Rahman, M., Ransom, S. M., Renard, A., Sanghavi, P., Scholz, P., Shaw, J. R., Shin, K., Siegel, S. R., Singh, S., Smegal, R. J., Smith, K. M., Stairs, I. H., Tendulkar, S. P., Tretyakov, I., Vanderlinde, K., Wang, H., Wang, X., Wulf, D., Yadav, P., Zwaniga, A. V., Massachusetts Institute of Technology. Department of Mechanical Engineering, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, CHIME/FRB Collaboration, Amiri, M., Andersen, B. C., Bandura, K. M., Bhardwaj, M., Boyle, P. J., Brar, C., Chawla, P., Chen, Ting, Cliche, J. F., Cubranic, D., Deng, M., Denman, N. T., Dobbs, M., Dong, F. Q., Fandino, M., Fonseca, E., Gaensler, B. M., Giri, U., Good, D. C., Halpern, M., Hessels, J. W. T., Hill, A. S., Hofer, C., Josephy, A., Kania, J. W., Karuppusamy, R., Kaspi, V. M., Keimpema, A., Kirsten, F., Landecker, T. L., Lang, D. A., Leung, Calvin, Li, D. Z., Lin, H.-H., Marcote, B., Masui, Kiyoshi, Mckinven, R., Mena Parra, Juan David, Merryfield, M., Michilli, D., Milutinovic, N., Mirhosseini, A., Naidu, A., Newburgh, L. B., Ng, C., Nimmo, K., Paragi, Z., Patel, C., Pen, U.-L., Pinsonneault-Marotte, T., Pleunis, Z., Rafiei- Ravandi, M., Rahman, M., Ransom, S. M., Renard, A., Sanghavi, P., Scholz, P., Shaw, J. R., Shin, K., Siegel, S. R., Singh, S., Smegal, R. J., Smith, K. M., Stairs, I. H., Tendulkar, S. P., Tretyakov, I., Vanderlinde, K., Wang, H., Wang, X., Wulf, D., Yadav, P., and Zwaniga, A. V.
Abstract: ast radio bursts (FRBs) are bright, millisecond-duration radio transients originating from sources at extragalactic distances, the origin of which is unknown. Some FRB sources emit repeat bursts, ruling out cataclysmic origins for those events. Despite searches for periodicity in repeat burst arrival times on timescales from milliseconds to many days these bursts have hitherto been observed to appear sporadically and—although clustered—without a regular pattern. Here we report observations of a 16.35 ± 0.15 day periodicity (or possibly a higher-frequency alias of that periodicity) from the repeating FRB 180916.J0158+65 detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project4,9. In 38 bursts recorded from 16 September 2018 to 4 February 2020 utc, we find that all bursts arrive in a five-day phase window, and 50 per cent of the bursts arrive in a 0.6-day phase window. Our results suggest a mechanism for periodic modulation either of the burst emission itself or through external amplification or absorption, and disfavour models invoking purely sporadic processes.
Published: 2020

32. Limits on the Ultra-bright Fast Radio Burst Population from the CHIME Pathfinder

Author: Amiri, M., primary, Bandura, K., additional, Berger, P., additional, Bond, J. R., additional, Cliche, J. F., additional, Connor, L., additional, Deng, M., additional, Denman, N., additional, Dobbs, M., additional, Domagalski, R. S., additional, Fandino, M., additional, Gilbert, A. J., additional, Good, D. C., additional, Halpern, M., additional, Hanna, D., additional, Hincks, A. D., additional, Hinshaw, G., additional, Höfer, C., additional, Hsyu, G., additional, Klages, P., additional, Landecker, T. L., additional, Masui, K., additional, Mena-Parra, J., additional, Newburgh, L. B., additional, Oppermann, N., additional, Pen, U. L., additional, Peterson, J. B., additional, Pinsonneault-Marotte, T., additional, Renard, A., additional, Shaw, J. R, additional, Siegel, S. R., additional, Sigurdson, K., additional, Smith, K., additional, Storer, E., additional, Tretyakov, I., additional, Vanderlinde, K., additional, and Wiebe, D. V., additional
Published: 2017
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33. HIRAX: a probe of dark energy and radio transients

Author: Newburgh, L. B., additional, Bandura, K., additional, Bucher, M. A., additional, Chang, T.-C., additional, Chiang, H. C., additional, Cliche, J.F., additional, Davé, R., additional, Dobbs, M., additional, Clarkson, C., additional, Ganga, K. M., additional, Gogo, T., additional, Gumba, A., additional, Gupta, N., additional, Hilton, M., additional, Johnstone, B., additional, Karastergiou, A., additional, Kunz, M., additional, Lokhorst, D., additional, Maartens, R., additional, Macpherson, S., additional, Mdlalose, M., additional, Moodley, K., additional, Ngwenya, L., additional, Parra, J. M., additional, Peterson, J., additional, Recnik, O., additional, Saliwanchik, B., additional, Santos, M. G., additional, Sievers, J. L., additional, Smirnov, O., additional, Stronkhorst, P., additional, Taylor, R., additional, Vanderlinde, K., additional, Van Vuuren, G., additional, Weltman, A., additional, and Witzemann, A., additional
Published: 2016
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34. THE Q/U IMAGING EXPERIMENT INSTRUMENT

Author: Bischoff, C., primary, Brizius, A., additional, Buder, I., additional, Chinone, Y., additional, Cleary, K., additional, Dumoulin, R. N., additional, Kusaka, A., additional, Monsalve, R., additional, Næss, S. K., additional, Newburgh, L. B., additional, Nixon, G., additional, Reeves, R., additional, Smith, K. M., additional, Vanderlinde, K., additional, Wehus, I. K., additional, Bogdan, M., additional, Bustos, R., additional, Church, S. E., additional, Davis, R., additional, Dickinson, C., additional, Eriksen, H. K., additional, Gaier, T., additional, Gundersen, J. O., additional, Hasegawa, M., additional, Hazumi, M., additional, Holler, C., additional, Huffenberger, K. M., additional, Imbriale, W. A., additional, Ishidoshiro, K., additional, Jones, M. E., additional, Kangaslahti, P., additional, Kapner, D. J., additional, Lawrence, C. R., additional, Leitch, E. M., additional, Limon, M., additional, McMahon, J. J., additional, Miller, A. D., additional, Nagai, M., additional, Nguyen, H., additional, Pearson, T. J., additional, Piccirillo, L., additional, Radford, S. J. E., additional, Readhead, A. C. S., additional, Richards, J. L., additional, Samtleben, D., additional, Seiffert, M., additional, Shepherd, M. C., additional, Staggs, S. T., additional, Tajima, O., additional, Thompson, K. L., additional, Williamson, R., additional, Winstein, B., additional, Wollack, E. J., additional, and Zwart, J. T. L., additional
Published: 2013
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35. HIRAX: a probe of dark energy and radio transients

Author: Hall, Helen J., Gilmozzi, Roberto, Marshall, Heather K., Newburgh, L. B., Bandura, K., Bucher, M. A., Chang, T.-C., Chiang, H. C., Cliche, J.F., Davé, R., Dobbs, M., Clarkson, C., Ganga, K. M., Gogo, T., Gumba, A., Gupta, N., Hilton, M., Johnstone, B., Karastergiou, A., Kunz, M., Lokhorst, D., Maartens, R., Macpherson, S., Mdlalose, M., Moodley, K., Ngwenya, L., Parra, J. M., Peterson, J., Recnik, O., Saliwanchik, B., Santos, M. G., Sievers, J. L., Smirnov, O., Stronkhorst, P., Taylor, R., Vanderlinde, K., Van Vuuren, G., Weltman, A., and Witzemann, A.
Published: 2016
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36. FIRST SEASON QUIET OBSERVATIONS: MEASUREMENTS OF COSMIC MICROWAVE BACKGROUND POLARIZATION POWER SPECTRA AT 43 GHz IN THE MULTIPOLE RANGE 25 ≤ ℓ ≤ 475.

Author: BISCHOFF, C., BRIZIUS, A., BUDER, I., CHINONE, Y., CLEARY, K., DUMOULIN, R. N., KUSAKA, A., MONSALVE, R., NÆSS, S. K., NEWBURGH, L. B., REEVES, R., SMITH, K. M., WEHUS, I. K., ZUNTZ, J. A., ZWART, J. T. L., BRONFMAN, L., BUSTOS, R., CHURCH, S. E., DICKINSON, C., and ERIKSEN, H. K.
Subjects: COSMIC background radiation, MEASUREMENT, OPTICAL polarization, ANISOTROPY, SYNCHROTRON radiation
Abstract: The Q/U Imaging ExperimenT (QUIET) employs coherent receivers at 43 GHz and 94 GHz, operating on the Chajnantor plateau in the Atacama Desert in Chile, to measure the anisotropy in the polarization of the cosmic microwave background (CMB). QUIET primarily targets the B modes from primordial gravitational waves. The combination of these frequencies gives sensitivity to foreground contributions from diffuse Galactic synchrotron radiation. Between 2008 October and 2010 December, over 10,000 hr of data were collected, first with the 19 element 43 GHz array (3458 hr) and then with the 90 element 94 GHz array. Each array observes the same four fields, selected for low foregrounds, together covering %1000 deg². This paper reports initial results from the 43 GHz receiver, which has an array sensitivity to CMB fluctuations of 69 µK√s. The data were extensively studied with a large suite of null tests before the power spectra, determined with two independent pipelines, were examined. Analysis choices, including data selection, were modified until the null tests passed. Cross-correlating maps with different telescope pointings is used to eliminate a bias. This paper reports the EE, BB, and EB power spectra in the multipole range ℓ = 25-475. With the exception of the lowest multipole bin for one of the fields, where a polarized foreground, consistent with Galactic synchrotron radiation, is detected with 3cr significance, the E-mode spectrum is consistent with the ACDM model, confirming the only previous detection of the first acoustic peak. The B-mode spectrum is consistent with zero, leading to a measurement of the tensor-to-scalar ratio of Due to image rights restrictions, multiple line equation(s) cannot be graphically displayed. The combination of a new time-stream "double-demodulation" technique, side-fed Dragoman optics, natural sky rotation, and frequent boresight rotation leads to the lowest level of systematic contamination in the B-mode power so far reported, below the level of r = 0.1. [ABSTRACT FROM AUTHOR]
Published: 2011
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37. The Q/U Imaging ExperimenT: Polarization Measurements of the Galactic Plane at 43 and 95 GHz

Author: Quiet, Collaboration, Ruud, T. M., Fuskeland, U., Wehus, I. K., Vidal, M., Araujo, D., Bischoff, C., Buder, I., Chinone, Y., Cleary, K., Dumoulin, R. N., Kusaka, A., Monsalve, R., Naess, S. K., Newburgh, L. B., Reeves, R. A., Zwart, J. T. L., Bronfman, L., Davies, R. D., Davis, R., Dickinson, C., Eriksen, H. K., Gaier, T., Gundersen, J. O., Hasegawa, M., Hazumi, M., Huffenberger, K. M., Jones, M. E., Lawrence, C. R., Leitch, E. M., Limon, M., Miller, A. D., Timothy Pearson, Piccirillo, L., Radford, S. J. E., Readhead, A. C. S., Samtleben, D., Seiffert, M., Shepherd, M. C., Staggs, S. T., Tajima, O., and Thompson, K. L.
Subjects: Physics, Spectral index, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Galactic Center, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, Polarization (waves), CMB cold spot, symbols.namesake, Space and Planetary Science, QUIET, symbols, Galactic coordinate system, Planck, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present polarization observations of two Galactic plane fields centered on Galactic coordinates (l,b)=(0 deg,0 deg) and (329 deg, 0 deg) at Q- (43 GHz) and W-band (95 GHz), covering between 301 and 539 square degrees depending on frequency and field. These measurements were made with the QUIET instrument between 2008 October and 2010 December, and include a total of 1263 hours of observations. The resulting maps represent the deepest large-area Galactic polarization observations published to date at the relevant frequencies with instrumental rms noise varying between 1.8 and 2.8 uK deg, 2.3-6 times deeper than corresponding WMAP and Planck maps. The angular resolution is 27.3' and 12.8' FWHM at Q- and W-band, respectively. We find excellent agreement between the QUIET and WMAP maps over the entire fields, and no compelling evidence for significant residual instrumental systematic errors in either experiment, whereas the Planck 44 GHz map deviates from these in a manner consistent with reported systematic uncertainties for this channel. We combine QUIET and WMAP data to compute inverse-variance-weighted average maps, effectively retaining small angular scales from QUIET and large angular scales from WMAP. From these combined maps, we derive constraints on several important astrophysical quantities, including a robust detection of polarized synchrotron spectral index steepening of ~0.2 off the plane, as well as the Faraday rotation measure toward the Galactic center (RM=-4000 +/- 200 rad m^-2), all of which are consistent with previously published results. Both the raw QUIET and the co-added QUIET+WMAP maps are made publicly available together with all necessary ancillary information., 22 pages, 18 figures; accepted for publication in ApJ; data are available on Lambda (http://lambda.gsfc.nasa.gov)

38. The QUIET Instrument

Author: Quiet, Collaboration, Bischoff, C., Brizius, A., Buder, I., Chinone, Y., Cleary, K., Dumoulin, R. N., Kusaka, A., Monsalve, R., Naess, S. K., Newburgh, L. B., Nixon, G., Reeves, R., Smith, K. M., Vanderlinde, K., Wehus, I. K., Bogdan, M., Bustos, R., Church, S. E., Davis, R., Dickinson, C., Eriksen, H. K., Gaier, T., Gundersen, J. O., Hasegawa, M., Hazumi, M., Holler, C., Huffenberger, K. M., Imbriale, W. A., Ishidoshiro, K., Jones, M. E., Kangaslahti, P., Kapner, D. J., Lawrence, C. R., Leitch, E. M., Limon, M., Mcmahon, J. J., Miller, A. D., Nagai, M., Nguyen, H., Timothy Pearson, Piccirillo, L., Radford, S. J. E., Readhead, A. C. S., Richards, J. L., Samtleben, D., Seiffert, M., Shepherd, M. C., Staggs, S. T., Tajima, O., Thompson, K. L., Williamson, R., Winstein, B., Wollack, E. J., and Zwart, J. T. L.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the Cosmic Microwave Background, targeting the imprint of inflationary gravitational waves at large angular scales (~ 1 degree). Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4 m side-fed Dragonian telescope. The polarimeters which form the focal planes use a highly compact design based on High Electron Mobility Transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 uK sqrt(s)) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r < 0.1. The 84-element W-band polarimeter array has a sensitivity of 87 uK sqrt(s) at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r < 0.01. The two arrays together cover multipoles in the range l= 25-975. These are the largest HEMT-based arrays deployed to date. This article describes the design, calibration, performance of, and sources of systematic error for the instrument.

39. SECOND SEASON QUIET OBSERVATIONS: MEASUREMENTS OF THE COSMIC MICROWAVE BACKGROUND POLARIZATION POWER SPECTRUM AT 95 GHz.

Author: Collaboration, QUIET, Araujo, D., Bischoff, C., Brizius, A., Buder, I., Chinone, Y., Cleary, K., Dumoulin, R. N., Kusaka, A., Monsalve, R., Næss, S. K., Newburgh, L. B., Reeves, R., Wehus, I. K., Zwart, J. T. L., Bronfman, L., Bustos, R., Church, S. E., Dickinson, C., and Eriksen, H. K.
Subjects: COSMIC background radiation, POLARIZATION (Nuclear physics), ASTROPHYSICAL radiation, GRAVITATIONAL waves, GRAVITATIONAL wave astronomy
Abstract: The Q/U Imaging ExperimenT (QUIET) has observed the cosmic microwave background (CMB) at 43 and 95 GHz. The 43 GHz results have been published in a previous paper, and here we report the measurement of CMB polarization power spectra using the 95 GHz data. This data set comprises 5337 hr of observations recorded by an array of 84 polarized coherent receivers with a total array sensitivity of 87 μK. Four low-foreground fields were observed, covering a total of ∼1000 deg2 with an effective angular resolution of 12.′8, allowing for constraints on primordial gravitational waves and high signal-to-noise measurements of the E-modes across three acoustic peaks. The data reduction was performed using two independent analysis pipelines, one based on a pseudo-Cℓ (PCL) cross-correlation approach, and the other on a maximum-likelihood (ML) approach. All data selection criteria and filters were modified until a predefined set of null tests had been satisfied before inspecting any non-null power spectrum. The results derived by the two pipelines are in good agreement. We characterize the EE, EB, and BB power spectra between ℓ = 25 and 975 and find that the EE spectrum is consistent with ΛCDM, while the BB power spectrum is consistent with zero. Based on these measurements, we constrain the tensor-to-scalar ratio to r = 1.1+0.9– 0.8 (r < 2.8 at 95% C.L.) as derived by the ML pipeline, and r = 1.2+0.9– 0.8 (r < 2.7 at 95% C.L.) as derived by the PCL pipeline. In one of the fields, we find a correlation with the dust component of the Planck Sky Model, though the corresponding excess power is small compared to statistical errors. Finally, we derive limits on all known systematic errors, and demonstrate that these correspond to a tensor-to-scalar ratio smaller than r = 0.01, the lowest level yet reported in the literature. [ABSTRACT FROM AUTHOR]
Published: 2012
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40. Atacama Cosmology Telescope: A Catalog of >4000 Sunyaev–Zel’dovich Galaxy Clusters

Author: Eli S. Rykoff, Jo Dunkley, E. Bertin, Ofer Lahav, Nick Battaglia, M. Soares-Santos, Hironao Miyatake, Shannon M. Duff, R. D. Wilkinson, Adriaan J. Duivenvoorden, L. N. da Costa, Joel N. Ullom, Robert Morgan, D. L. Burke, Devin Crichton, Kavilan Moodley, Peter Doel, Alexandra Amon, Edward J. Wollack, N. C. Robertson, H. T. Diehl, Joseph E. Golec, Sunayana Bhargava, Samuel Hinton, Emmanuel Schaan, Enrique Gaztanaga, Megan Gralla, David N. Spergel, Johannes Hubmayr, Simon Dicker, David Bacon, S. Allam, Robert A. Gruendl, Simone Ferraro, C. Aros-Bunster, Felipe Menanteau, G. Gutierrez, Kevin M. Huffenberger, Daniel Thomas, Ramon Miquel, Michael D. Niemack, I. Ferrero, Mathew S. Madhavacheril, J. P. Dietrich, Niall MacCrann, Juan Garcia-Bellido, Tesla E. Jeltema, David J. James, Yanxi Zhang, A. K. Romer, Ben Hoyle, Hy Trac, Mark J. Devlin, Patricio A. Gallardo, J. Gschwend, A. A. Plazas, Brian J. Koopman, Rolando Dünner, Zhilei Xu, Simone Aiola, Behzad Ansarinejad, A. Choi, Jeff McMahon, Eduardo Rozo, Gary Bernstein, K. Honscheid, Michel Aguena, Tanay Bhandarkar, Dan Becker, C. Sifon, Neelima Sehgal, Bhuvnesh Jain, Laura Newburgh, Dongwon Han, F. Paz-Chinchón, J. R. Bond, Kyler Kuehn, Peter Melchior, M. Carrasco Kind, Eve M. Vavagiakis, Steve K. Choi, Suzanne T. Staggs, Paul Giles, R. L. C. Ogando, J. C. Hill, Federico Nati, M. E. C. Swanson, E. V. Denison, Kevin T. Crowley, Tony Mroczkowski, W. G. Hartley, Antonella Palmese, Martine Lokken, S. Kent, Alessandro Schillaci, Masamune Oguri, John P. Hughes, M. A. G. Maia, Maria Salatino, S. Amodeo, T. Shin, S. Adhikari, M. Hasselfield, M. Costanzi, S. I. Loubser, J. Van Lanen, B. Partridge, Sigurd Naess, Adam D. Hincks, J. A. Beall, B. Flaugher, S. M. Simon, Jason E. Austermann, S. P. Ho, John Orlowski-Scherer, M. Smith, Daniel Gruen, J. Martin, D. W. Gerdes, J. Annis, Kenda Knowles, David J. Brooks, Erminia Calabrese, Emilie R. Storer, Gene C. Hilton, Leila R. Vale, Salcedo Romero de Ávila, Phumlani Phakathi, Josh Frieman, Yen-Ting Lin, T. M. C. Abbott, Chun-Hao To, E. J. Sanchez, J. Carretero, E. Suchyta, Matt Hilton, Christopher J. Conselice, Tobias A. Marriage, Sebastian Grandis, A. Carnero Rosell, Agnès Ferté, Anton T. Jaelani, Marcos Lima, S. Everett, S. Serrano, Lyman A. Page, J. De Vicente, Atsushi J. Nishizawa, G. Tarle, UAM. Departamento de Física Teórica, Hilton, M, Sifon, C, Naess, S, Madhavacheril, M, Oguri, M, Rozo, E, Rykoff, E, Adhikari, S, Aguena, M, Aiola, S, Allam, S, Amodeo, S, Amon, A, Annis, J, Ansarinejad, B, Abbott, T, Aros-Bunster, C, Austermann, J, Avila, S, Bacon, D, Battaglia, N, Beall, J, Becker, D, Bernstein, G, Bertin, E, Bhandarkar, T, Bhargava, S, Bond, J, Brooks, D, Burke, D, Calabrese, E, Carrasco Kind, M, Carretero, J, Choi, S, Choi, A, Conselice, C, Da Costa, L, Costanzi, M, Crichton, D, Crowley, K, Dunner, R, Denison, E, Devlin, M, Dicker, S, Diehl, H, Dietrich, J, Doel, P, Duff, S, Duivenvoorden, A, Dunkley, J, Everett, S, Ferraro, S, Ferte, A, Flaugher, B, Frieman, J, Ferrero, I, Gallardo, P, Garcia-Bellido, J, Gaztanaga, E, Giles, P, Golec, J, Gralla, M, Grandis, S, Gruen, D, Gerdes, D, Gruendl, R, Gschwend, J, Gutierrez, G, Han, D, Hartley, W, Hasselfield, M, Hill, J, Hilton, G, Hincks, A, Hinton, S, Ho, S, Honscheid, K, Hoyle, B, Hubmayr, J, Huffenberger, K, Hughes, J, Jaelani, A, Jain, B, James, D, Jeltema, T, Kent, S, Knowles, K, Koopman, B, Kuehn, K, Lahav, O, Lima, M, Lin, Y, Lokken, M, Loubser, S, Maccrann, N, Maia, M, Marriage, T, Martin, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Moodley, K, Morgan, R, Mroczkowski, T, Nati, F, Newburgh, L, Niemack, M, Nishizawa, A, Miyatake, H, Ogando, R, Orlowski-Scherer, J, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Phakathi, P, Plazas, A, Robertson, N, Romer, A, Carnero Rosell, A, Sanchez, E, Schaan, E, Schillaci, A, Sehgal, N, Serrano, S, Shin, T, Simon, S, Smith, M, Salatino, M, Soares-Santos, M, Spergel, D, Staggs, S, Storer, E, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Trac, H, Ullom, J, Vale, L, Van Lanen, J, Vavagiakis, E, De Vicente, J, Wilkinson, R, Wollack, E, Xu, Z, Zhan, Y, Hilton, M., Sifón, C., Naess, S., Madhavacheril, M., Oguri, M., Rozo, E., Rykoff, E., Abbott, T. M. C., Adhikari, S., Aguena, M., Aiola, S., Allam, S., Amodeo, S., Amon, A., Annis, J., Ansarinejad, B., Aros-Bunster, C., Austermann, J. E., Avila, S., Bacon, D., Battaglia, N., Beall, J. A., Becker, D. T., Bernstein, G. M., Bertin, E., Bhandarkar, T., Bhargava, S., Bond, J. R., Brooks, D., Burke, D. L., Calabrese, E., Carretero, J., Choi, S. K., Choi, A., Conselice, C., da Costa, L. N., Costanzi, M., Crichton, D., Crowley, K. T., Dünner, R., Denison, E. V., Devlin, M. J., Dicker, S. R., Diehl, H. T., Dietrich, J. P., Doel, P., Duff, S. M., Duivenvoorden, A. J., Dunkley, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giles, P., Golec, J. E., Gralla, M. B., Grandis, S., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Han, D., Hartley, W. G., Hasselfield, M., Hill, J. C., Hilton, G. C., Hincks, A. D., Hinton, S. R., S-P. P., Ho, Honscheid, K., Hoyle, B., Hubmayr, J., Huffenberger, K. M., Hughes, J. P., Jaelani, A. T., Jain, B., James, D. J., Jeltema, T., Kent, S., Carrasco Kind, M., Knowles, K., Koopman, B. J., Kuehn, K., Lahav, O., Lima, M., Lin, Y-T., Lokken, M., Loubser, S. I., Maccrann, N., Maia, M. A. G., Marriage, T. A., Martin, J., Mcmahon, J., Melchior, P., Menanteau, F., Miquel, R., Miyatake, H., Moodley, K., Morgan, R., Mroczkowski, T., Nati, F., Newburgh, L. B., Niemack, M. D., Nishizawa, A. J., Ogando, R. L. C., Orlowski-Scherer, J., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Phakathi, P., Plazas, A. A., Robertson, N. C., Romer, A. K., Carnero Rosell, A., Salatino, M., Sanchez, E., Schaan, E., Schillaci, A., Sehgal, N., Serrano, S., Shin, T., Simon, S. M., Smith, M., Soares-Santos, M., Spergel, D. N., Staggs, S. T., Storer, E. R., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Trac, H., Ullom, J. N., Vale, L. R., Van Lanen, J., Vavagiakis, E. M., De Vicente, J., Wilkinson, R. D., Wollack, E. J., Xu, Z., and Zhang, Y.
Subjects: Galaxy clusters, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Large-scale structure of the universe, Astrophysics - Cosmology and Nongalactic Astrophysics, Intracluster medium, 0103 physical sciences, Cluster (physics), Sunyaev-Zeldovich Effect, 010303 astronomy & astrophysics, Cosmology, Galaxy clusters, Galaxy cluster, Astrophysics::Galaxy Astrophysics, AGLOMERADOS (GALÁXIA), Physics, 010308 nuclear & particles physics, Star formation, Física, Astronomy and Astrophysics, XMM-newton Telescope, Galaxies, Galaxy, Redshift, Space and Planetary Science, Atacama Cosmology Telescope
Abstract: Hilton, M., et al., We present a catalog of 4195 optically confirmed Sunyaev–Zel’dovich (SZ) selected galaxy clusters detected with signal-to-noise ratio >4 in 13,211 deg of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multifrequency matched filter to 98 and 150 GHz maps constructed from ACT observations obtained from 2008 to 2018 and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04 < z < 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ signal versus mass-scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M > 3.8 × 10 M, evaluated at z = 0.5, for clusters detected at signal-to-noise ratio >5 in maps filtered at an angular scale of 2 4. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ signal mass-scaling relation, such as the Dark Energy Survey (4566 deg), the Hyper Suprime-Cam Subaru Strategic Program (469 deg), and the Kilo Degree Survey (825 deg). We highlight some noteworthy objects in the sample, including potentially projected systems, clusters with strong lensing features, clusters with active central galaxies or star formation, and systems of multiple clusters that may be physically associated. The cluster catalog will be a useful resource for future cosmological analyses and studying the evolution of the intracluster medium and galaxies in massive clusters over the past 10 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

41. 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

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